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Photon Detection with Superconducting Detectors from Millimeter-Wave to Gamma-Ray Presented by: About Us The Photonic Detection technical group is part of the Photonics and Opto- Electronics Division of the Optical Society. This group focuses

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Photon Detection with Superconducting Detectors from Millimeter-Wave to Gamma-Ray

Presented by:

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The Photonic Detection technical group is part of the Photonics and Opto- Electronics Division of the Optical Society. This group focuses on the detection of photons as received from images, data links, and experimental spectroscopic studies to mention a few. Within its scope, the PD technical group is involved in the design, fabrication, and testing of single and arrayed detectors. This group focuses on materials, architectures, and readout circuitry needed to transduce photons into electrical signals and further processing. This group’s interests include: (1) the integration of lens, cold shields, and readout electronics into cameras, (2) research into higher efficiency, lower noise, and/or wavelength tunability, (3) techniques to mitigate noise and clutter sources that degrade detector performance, and (4) camera design, components, and circuitry.

About Us

Shayan Garani Srinivasa, Chair (Indian Institute of Science), shayan.gs@dese.iisc.ernet.in Francesco Marsili, Vice Chair (JPL), francesco.marsili.dr@jpl.nasa.gov Rajesh Nair, Treasurer (Indian Institute of Technology Ropar), rvnair@iitrpr.ac.in Supriyo Bandyopadhyay, Committee (VA Commonwealth University), sbandy@vcu.edu Lingze Duan, Committee (University of Alabama in Huntsville), lingze.duan@uah.edu

Executive Board

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LinkedIn Group

www.linkedin.com/groups/Photonic- Detection-Technical-Group-8297763/about

Find us online OSA Homepage

www.osa.org/PD

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Our activities include:

  • Special sessions at leading OSA conferences. We had a successful panel discussion at OSA FiO 2015.
  • Webinars. We have planned about 3-4 webinars for 2016.
  • Proposal on a journal special issue covering PD activities.
  • Interaction with local sections and student chapters. We are in the process of setting this up.
  • Proposal for the creation of student poster awards at OSA meetings.
  • Road map towards solving outstanding research problems.

Outreach:

  • Regular communications (distribution list announcements and listservs)
  • Create and maintain an active/engaged social media/networking functions (e.g., SharePoint, Google Plus,

Twitter, Facebook, and/or LinkedIn).

Planned Technical Group Activities

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Detecting photon with superconducting detectors from millimeter-wave to gamma-ray

Jiansong Gao Quantum Sensors Group National Institute of Standards and Technology Boulder, CO

OSA webinar, 9/28/2016

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  • Electrical resistance goes to zero at

a critical temperature Tc

  • Critical Current Ic or density Jc

above which there is resistance

  • Electrons in the superconducting

ground state form Cooper pairs

  • Excitations above the ground state

are known as quasi-particles, energy ~ 2Δ

0.02 0.04 0.06 95.8 96 96.2

Temperature (mK)

Resistance (W)

Superconductivity

N E

hn>2D

Operating at T~Tc, it is an extremely sensitive thermometer. Operating at T<<Tc, it is like a “semiconductor” with extremely small gap Al: Tc=1.2K, Δ ~ 0.0002 eV Nb: Tc = 9.2K, Δ ~ 0.0014 eV Si gap ~ 1.1eV

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Why superconducting detectors

  • Low noise
  • Johnson noise: 4kTR
  • High sensitivity, low cutoff frequency
  • Superconductor gap ~1 meV v.s. semiconductor gap ~1eV
  • We are effectively using a ruler with finer mark.
  • In quantum picture, most detectors works by counting some kind of

quanta (e.g., phonons or electron excitations) in a system.

hn

  • 1, T1, V1

T3 <T2 5 < 1 T2 <T1

Smallest size of quanta, smallest volume, lowest temperature = Highest sensitivity T1 T2 T3 T4

T4 <T1 , V1 <V0

1 2 3 4 5 T

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Superconducting v.s. conventional detectors: an example

TES

Energy-dispersive gamma-ray detectors conventional Semiconductor detectors Superconducting transition edge sensors (TES)

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Superconducting photodetectors – by wavelength

Cosmic Microwave Background (CMB) THz security imaging Photon counting for quantum

  • ptics/information/communication

X-ray imaging/spectroscopy for material analysis gammy-ray imaging/spectroscopy for nuclear material analysis

0.4 meV (90 GHz) 100 keV

Cosmology, astronomy, astrophysics

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Superconducting detectors - by mode of operation

  • Bolometer - measuring power
  • Calorimeter – counting photons
  • Energy not resolved
  • Energy resolving (photon number resolving)

t A t A NEP: Noise equivalent power DE: Energy resolution

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Superconducting detectors — by technology

  • Superconducting tunnel junction detector (STJ)
  • Superconducting nanowire single photon detector (SNSPD)
  • Superconducting transition edge sensor (TES)
  • Microwave kinetic inductance detector (MKID)

Most of the detectors shown in this talk are developed at NIST (Boulder) Quantum Sensors (Joel Ullom): MM, THz, X-ray, Gamma-ray TES and MKID Single Photonics and Quantum Information (Sae Woo Nam): NIR, optical TES and SNSPD

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X-ray Photon Cooper Pairs Excess Charge

Signal = Current Pulse

Nb Nb Al Al Al2O3 Tunnel Barrier EF DNb DAl

Al2O3

  • 100  100 µm

SiO2 Nb Nb Absorber (165 nm) Al Si Substrate SiO2 Al Nb X-ray Photon

  • Analogous to a semiconductor detector
  • Energy resolving
  • Al – AlOxide – Al junctions
  • JJ not popular as detector – hard to scale to a large array
  • building block for SQUIDs and quantum bits (qubits)

Superconducting tunnel junction detector (STJ)

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Superconducting nanowire single photon detector (SNSPD)

  • NbN, Wsi, … 4nm thick, <50nm wide
  • Current bias, voltage pulse
  • Photon counting, but not energy resolving
  • Fastest superconducting detector, ~50ps jitter
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0.06 96 96.2

temperature (mK) resistance (Ω)

0.00 95.8

thin-film thermometer TES micrograph SiN current

Transition Edge Sensors (TES)

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TES bolometer for cosmic ray background (CMB)

TES

Gold meander SiN legs Nb (GND)

NIST dual polarization TES for ABS, SPTPol, ACTPol

TES BPF

Feedhorn array

Application - Cosmology

TES: AlMn (Tc~500mK), MoCu (Tc~150mK), feedhorn-coupled B-mode polarization in the CMB is a signature of gravity waves and the energy scale of inflation. B-mode lensing detected SPTPol (using NIST TES detectors) in 2013 temperature anisotropy (1992) E-mode polarization (2002)

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TES for THz imaging

  • TES: Al (Tc~1.2K), feedhorn-coupled
  • Passive thermal imaging at 350GHz
  • 17 m standoff distance
  • 6 fps video for live imaging
  • 1 cm spatial and 0.1 K temperature resolution

Application - Security 17 m

Credit: Dan Becker

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Visible/IR single photon counting TES

  • Photon Number Resolution
  • >95% end-to-end measured

efficiency at 1550nm

1000 2000 3000 4000 5000 6000 7000 1000 2000 3000 4000 5000 6000

Pulse Height (MCA bins) Counts (a.u.)

n=1 n=2 n=3 n=11 n=4 n=5 n=6 n=7 n=10 n=8 n=9 Application – Quantum information

TES: W (Tc~100 mK), fiber coupled

Credit: Sae Woo Nam, Adriana Lita

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  • 2.5 eV resolution at 6 keV
  • X-ray TES, MoCu 100mK, Au or Bi

TES X-ray spectroscopy

  • Uranium chemical shifts

(Los Alamos/STAR Cryo commercial system )

  • 240 TES instrument installed at APS

Application – Material analysis

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19 TES: MoCu (Tc~150mK), Sn absorber Application – Nuclear material analysis

TES g-ray spectroscopy

Sn TES g-ray spectroscopy: high res., fast, in-situ to replacing mass spectrometry: slow, destructive

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TES readout and scaling to large arrays

bias wire + SQUID readout wire Time Domain SQUID Multiplexer

  • Currently TDM, FDM, CDM

utilizes MHz bandwidth To scale to large detector array

  • Less wires
  • More bandwidth

Microwave readout

Largest TES instrument SCUBA-2: 10,000 TES TDM readout, still >2500 wires

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Microwave Kinetic Inductance Detectors (MKIDs)

  • Use superconducting resonators to sense quasiparticles

CPW: coplanar waveguide readout tone Invented by J. Zmuidzinas and H. Leduc at Caltech/JPL in 2000. Vin Vout Al, Nb, …

  • Kinetic Inductance of superconductor

* * 2 2 2

1 1 1 2 2 2

m m ki

E E n m v dr L I L I    

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Frequency domain multiplexing

In Out

HEMT

GHz bandwidth, 1000s of MKIDs needs one HEMT and one pair of coaxial cables!

Broadband low-noise amplifier Digital readout – 500MHz AD/DA

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TiN film ideal for MKID

Leduc, etal, APL 97, 102509 (2010), Vissers, etal , APL 97, 232509 (2010)

  • > multiplexing
  • > gap engineering
  • > good absorber
  • > responsivity

Advantages:

  • High kinetic inductance (100 times Al)
  • Low loss, Qi>107
  • High normal resistivity, rn~ 100 mW∙cm
  • Tunable Tc (0 – 5K)

Si substrate TiN TiN TiN TiN Ti Ti TiN trilayer

Credit: Mike Vissers

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TiN MKID photon counting at 1550 nm

Credit: Yiwen Wang (unpublished) Southwest Jiaotong University, China

  • J. Gao et al., APL 101, 142602 (2013)

TiN, Tc~0.9K, ΔE ~ 0.4 eV

1 2 3 4 5 6 7 8 9 ?

2012 TiN/Ti/TiN, Tc~1.4K, ΔE ~ 0.25 eV 2016

TiN Al

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Feedhorn-coupled MKID polarimeters/bolometers

  • Feedhorn-coupled, dual-

polarization sensitive.

  • Dual polarization

(a)

Feedhorn microstrip feedline Si cutout for

  • backshort

(SiO2 removed) IDC inductor strips SiO2 interface Nb radiation

in

  • ut
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Lab test using blackbody source

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Detector sensitivity

  • Lab blackbody load test has demonstrated photon-noise limited sensitivity

at 1.2 THz (250 mm).

1

Hubmayr et al, APL 106, 073505 (2015).

  • Excellent cross-pol rejection
  • Photon (shot) noise
  • Response to THz photon

Credit: Johannes Hubmayr

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+ +

template pixel tile … feedline winding tiles IDC triming mask

  • New “tiling and trimming” layout/fabrication scheme efficiently uses the stepper

to produce arbitrary-size (number of pixels, wafer size, pixel placement) high quality MKID arrays

MKID array design kit

MKID array fabrication

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MKID arrays for BLAST

3 rhombuses, 306 pixels/rhombus 1812 MKIDs

250um array

  • Yield close to 100%, 20% collision (5 bandwidth exclusion)
  • Qi ~ 500k@50mK, Qi ~ 40,000 under 17pW loading

Rhombus A

Credit: Chris Mckenney

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MKID polarimeters for BLAST-TNG

  • BLAST: Balloon-borne Large Aperture Submillimeter Telescope
  • 1.8 m mirror
  • feedhorn coupled
  • 3 arrays, 250, 350, and 500µm
  • study star formation
  • PI: Upenn + collaborators

BLAST BLAST-Pol BLAST-TNG 270 NTD detectors 2006 BLAST + Single Pol. 2010 3000 MKID Dual –pol detector 2017

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Research frontier

  • Better performance
  • Nanowire: higher efficiency, photon number resolving, multiplexing
  • TES: faster, better NEP or energy resolution
  • MKID: better NEP or energy resolution
  • Scaling to larger detector arrays: 1-1000 => 100,000 - 1M pixels
  • Fabrication: 3-4 inch -> 6 inch wafer
  • Readout: TDM -> microwave readout
  • Refrigeration: more compact size, larger cooling power, lower cost

Detected by SPTPol in 2013 To detect the Primordial B-mode signal, CMB4 project proposes 500,000 detectors (multiple arrays) deployed

  • n multiple telescopes to jointly observe for 3 years!!!