次世代サブミリ波天文観測装置DESHIMAの開発と実験室での性能評価

2016/11/24 KEK 測定器開発室セミナー
Kenichi Karatsu, Akira Endo, David Thoen,
Nuri van Marrewijk, Ozan Yurdseven, Nuria Llombart,
Teun Klapwijk, Jochem Baselmans
Vignesh Murugesan, Stephen Yates, Juan Bueno,
Jochem Baselmans
Nozomu Tomita, Shun Ishii, Kotaro Kohno
Tatsuya Takekoshi, Tai Oshima
1

Contents
Introduction
Submm astronomy
DESHIMA
DESHIMA
On-chip Filterbank Spectrometer
MKID
Cryogenic System
OpticsReadout
Experimental Results2Credit: STScI/JHU/NASA3

Credit: http://www.ccatobservatory.org/docs/ccat-reports-publications/Giovanelli-CCAT.pdf

VisibleInfraredSubmm

Credit: STScI/JHU/NASA4

Credit: STScI/JHU/NASA5

Microwave, Radio
Wavelength: 10-1 – 10-4 m, > 0.1 m
Freq.: 3×109 – 3×1012 Hz, < 3×109 Hz
CMB
Submm galaxies (Star formation)
Quasars

Credit: STScI/JHU/NASA6

Credit: STScI/JHU/NASA
7

Curiosity:
Evolution of galaxies, in the Cosmic Large Scale Structure(Kravtsov et al.)(Obreschkow 2009)‘Submm Galaxies’- Aggressive Star Formation:
Important ingredient forcosmic star-formation history
and evolution of galaxies- Dust extinction—> diﬃcult to detect in vis-NIR
Thermal reemission from dust—> Bright at THz-submm

flux density Jy- Galaxies found in
submillimeter-wave surveys

C+ 1.9 THz[CII] 1.9 THz linefrom galaxies

5000
O
O2+
O2+
S2+

N2+

O

Si+
S2+

1

3

10
frequency THz

What mysteries will we solve?
- Cosmic Star Formation History- Evolution of Galaxies- Cosmic Structure Formation
8

Bottleneck:Redshift measurement of submillimeter galaxies

Vis-NIR：

Submm：

Extremely faint because of
dust extinction

The effect of FIR lines o
No wideband spectrometer

Umehata et al. 2015

Submm
(ALMA)

Vis-NIR(Subaru)

Smail et al., Figure
2011 3. The

ALMA (8 GHz)

Figure 2. The rest-frame SED of SMM J2135−0102, a typical high-redshift
SMG at z = 2.3259, showing the bright, narrow molecular and atomic emission lines seen in the FIR and submillimetre. The continuum component of
the SED is derived from fits to the Herschel and ground-based photometry(Ivison et al. 2010a; Swinbank et al. 2010) corrected for the emission-line
contributions. Added to this are the emission lines derived from the observations of Danielson et al. (2011) or for lines shortward of 100 µm fromthe predictions from the PDR model used in that work. The observed [C II]
line in this source contributes 0.27 per cent of LFIR and along with otherstrong lines may make a significant contribution to broad-band fluxes at certain redshifts (to better illustrate this, the inset shows the same SED arounduum emission
bands, from[C II] 158 µm
z ∼ 0.6, 1.2, 2
fluxes of 5–10
line comprisin
will scale line
L[C II] /LFIR !
equal to four tflux scale. We
in the shorter9
respectively) a

TU Delft/SRON Breakthrough for Panoramic
3D view of the THz Universe:
No wide-field imager（A-MKID breakthrough）

No wideband spectrometer（DESHIMA breakthrough）
The effect of FIR lines

A-MKID(25,000 beams)
ALMA(FoV: ~10 arcsec)

A-MKID(25,000 pixel)

Smail et al., Figure
2011 3. T
Figure 2. The rest-frame SED of SMM J2135−0102, a typical high-redshift
SMG at z = 2.3259, showing the bright, narrow molecular and atomic emission lines seen in the FIR and submillimetre. The continuum component of
the SED is derived from fits to the Herschel and ground-based photometry(Ivison et al. 2010a; Swinbank et al. 2010) corrected for the emission-line
contributions. Added to this are the emission lines derived from the observations of Danielson et al. (2011) or for lines shortward of 100 µm fromthe predictions from the PDR model used in that work. The observed [C II]
line in this source contributes 0.27 per cent of LFIR and along with otherstrong lines may make a significant contribution to broad-band fluxes at cer-

ALMA (8 GHz)

(Vis: >1 Gpixel)(480 GHz)uum emissi
bands, from[C II] 158 µz ∼ 0.6, 1.2
fluxes of 5–line compri
will scale l
L[C II] /LFIR
equal to fou
flux scale. W
in the10shortProbing the cosmic history ofStar- and Galaxy-Formation in THz
Imaging camera → 2D projection

2D projection✴ The 3rd dimension = distance (time)

Galaxies in
3D space

DESHIMA
Deep Spectroscopic High-redshift Mapper
Delft SRON High-redshift Mapper

distance (time)

Goal: 3D map of
massive star-forming galaxies(Bright in the THz)
11

Idea:
Sorting THz photons by their age(1 Gyr = 109 years)
5.0 Gyr

5.5 Gyr

6.0 Gyr

6.5 Gyr

7.0 Gyr

7.5 Gyr

8.0 Gyr

8.5 Gyr

9.0 Gyr12

Idea:
Sorting THz photons by their wavelength(1 Gyr = 109 years)
5.0 Gyr

5.5 Gyr

6.0 Gyr

6.5 Gyr

7.0 Gyr

7.5 Gyr

8.0 Gyr

8.5 Gyr

9.0 Gyr13

Microwave Trick:

λ1

Photon sorting with superconducting micro-filters~500 filters

100 µm

λ2

λ2/2
λ1/2

Filters

λ4/2
λ3

λ3/2

λ4
Signal fromthe sky

To separate
detectors

14

Concept:
Superconducting On-chip Filterbank Spectrometer

DESHIMA [CII] survey
Filter:Signal Frequency

widebandsignal905 903.2 901.4
GHz GHz GHz

Microwave Readout(4-6 GHz)

327.2 326.6 326
GHz GHz GHz

antenna(lens in behind)~500
channels
6.000
5.996
GHz
5.992
GHz
GHz

NbTiN
Al

MKID:
ReadoutFrequency(absorber)

4.008
GHz 4.0044.000
GHz
GHz

No metal

15

DESHIMA- Filterbank chip
- F = 326-905 GHz (redshift 1-5 for [CII] 1.9 THz)
- F/ΔF = 500- Max 7 spatial pixels- Cryogenics: 2-stage ADR + 2-stage PTC

Microwave Readout(4-6 GHz)

Submm signal(326-906 GHz)
antenna(lens in behind)~500 channels

Microwave Kinetic Inductance Detector
NbTiN
AlNo metal

Filterbank chip @ 100 mK- 4000 MKID detectors, read out with 1 pair of coax
cables- Optics: 2x parabolic mirrors (M=1)

Absorber

Submm wave bandpass ﬁlter

Lens + chip (150 mK)

150 mK box
LPFx2 (150 mK)

double layer magnetic shieldcoax filters

Polarizer

800 mK intermediate stage- Compatible with ASTE and APEX telescopes inChile (5 km alt.)

LPF

pupil LPF
parabolic mirror x 2

collimating lens

LPF

4K
50K 300K
IR blockers/shaders

Figure 5. Cross section of the optical/thermal/mechanical structure of DESHIMA.

Cryo-optical assembly(100 mK, 800 mK, 3.5K)

16

DESHIMA

ASTE

on

7 spatial pixels (maximum)
θFWHM = 23.6ʺ @ 326 GHz, 8.5ʺ@ 906 GHz

Deep Spectroscopic
High-z Mapper‘1st light demo’‘maximum’θFWHM = 23.6ʺ @ 326 GHz, 8.5ʺ@ 906 GHzF

326-368 GHz

57’’

326-905 GHz[ Unique Selling Points ]✴ Ultra-broadband spectroscopy

SCUBA-2 850 µm✴ Photon-noise limited sensitivity

F/ΔF

500

500
towards a larger✴ Scalable concept,
instrument that will spectroscopicallyresolve the complete CIB(MOSAIC)

Npixels

1-2

max 7

NKIDs

100-200

max 4,000

60°

EL range

ASTE telescope(Atacama desert, 4800 m)[ Sensitivity ]
−17

m−2)

10

single shot!

[ Key Applications ]Rapid redshift searches
DESHIMA on ASTE will provide a deeper and more complete redshiftsearch than ALMA in the same observing time. The power of blind
redshift searches in the submm has recently been shown by Vieira et al17

Contents
Introduction
Submm astronomy
DESHIMA
DESHIMA
On-chip Filterbank Spectrometer
MKID
Cryogenic System
OpticsReadout
Experimental Results
18

320-370 GHz filterbank chip(# this photograph is 1 generation older)

CPW line

Various test

(S=W=0.5µm)

resonators

MKIDs

Antenna

Filterbank(64 channels, F/ΔF = 500)

Cosmology with Nanotechnology

Filter bank design
Interdigitated Capacitor Filter

film thickness: 100 nm
You can look at it as a meandered slot line…

from antenna(or previous filter)to next filter… or as an LC circuit.

L
short

bridge(PEC on vacuum)

NbTiN 100 nm(Ls = 1 pH/sq)
on c-plane SapphireC
to KIDL
20

Transmission

1st harmonic"

Interdigitated Capacitor Filter

2nd harmonic!

3rd harmonic"

21

The charge distribution over the resonator
Fundamental (1/2 x λ) mode

2nd harmonic (1 x λ)
(The ‘good’ one)

3rd harmonic (3/2 x λ)22

Why does the 2nd harmonic show low
radiation loss??
- Top and bottom resemble
2 dipoles with opposite polarity.
- Eﬃcient cancellation of radiation?

+

-

-

+

23

320-370 GHz filterbank chip(# this photograph is 1 generation older)

CPW line

Various test

(S=W=0.5µm)

resonators

MKIDs

Antenna

Filterbank(64 channels, F/ΔF = 500)

Cosmology with Nanotechnology

open end of the resonator, is a wide CPW made entirely fromIn the next decades millimeter and sub-mm astronomy
1
200 nm thick NbTiN. NbTiN has 10 dB lower TLS noise than
ire large format imaging arrays to complement theconventional superconductors such as Al.9 The TLS noise isspatial resolution of the Atacama Large Millimeter/
further reduced by the width of the CPW,9 23.7 lm and 5.4 lm
millimeter Array.2 The desired sensors should have aground limited sensitivity and a high optical efficiency
for the CPW gap and central line, respectively.
enable arrays of up to megapixels in size. The mostThe second section (1 mm), at the shorted end of the resmising candidates to fulfill these requirements are microonator, is a narrow CPW with NbTiN groundplanes and a
3
Full
NbTiN
CPW
e kinetic inductance detectors (MKIDs) due to their in48 nm thick Al central line. The Al isgalvanically connected
Al/NbTiN
CPW
nt potential for frequency domain multiplexing.
and the NbTiN~4MKIDs
mm to the NbTiN central line (Fig. 1, inset)~1mm
superconducting resonators, thousands of which can begroundplane at the resonator short. The NbTiN is lossless forpled to a single feedline. Each resonator is sensitive tofrequencies up to the gap 2D0 =h ¼ 1:1 THz ðTc ! 14 KÞ.
Any radiation with a frequency 0:09 < ! < 1:1 THz is thereges in the Cooper pair density induced by absorption offore absorbed in the Al (Tc ¼ 1.28 K) central line of the secmm radiation. By monitoring the change in either phaseond section. The optically excited quasiparticles are trapped
mplitude of the complex feedline transmission at thein the Al because it is connected to a high gap superconducID resonance one can measure the absorbed photon
tor. This quantum well structure confines the quasiparticles in
er. Using amplitude readout photon noise limited per4
mance has been shown. However, for practical applicas two key properties need to be demonstrated: (1) Photon
e limited operation in phase readout. (2) A measurement
e aperture efficiency,5 which describes the absolute optioupling of a MKID imaging array to a plane wave.
In this letter we present antenna coupled hybrid NbTiNMKIDs designed for groundbased sub-mm astronomy. We
Readout
5 noiseGHzlimited performw that these devices
achieve photon
in both amplitude andphase readout.
ThroughlineThrough a detailed
ysis of the optical coupling within our setup we validate
imulation of the lens-antenna far field beam pattern. From
we derive an aperture efficiency of 75%. This is close toheoretical maximum of 80% for a single-moded detector.
The device design, shown in Fig. 1, aims to simultaney maximize the phase response and minimize the two-levelem (TLS) noise contribution.8 The device is a L ! 5 mm
FIG. 1. Scanning electron micrograph of the antenna-coupled hybridIt’sessentiallythesameas this NbTiN/Al hybrid KID
quarter wavelength coplanar waveguide (CPW) resonator
NbTiN-Al MKIDs used. A wide NbTiN CPW resonator is used to minimize
the two-levelsystem noise
not meandered,antenna=> contribution.
filter) At the shorted end where the planar
isting of two sections. The(justfirst section("4 mm), at the and

350 GHz CPW filter + KID channel

KID

tronic mail: r.m.j.janssen@tudelft.nl

Filtersubmm
signalantenna is located, one millimeter of CPW is reduced in width, and the central line is made from thin Al. The Al is galvanically connected to the
NbTiN at both ends (inset).
C

25

Detector Technology✓ MKID = Microwave-Kinetic-Inductance-Detector:
Detect photons from changes in surface impedance (Zs) of superconducting
resonators
Readout signal~5 GHzwith photon

fr

Easy to read out large
number of channels (>1000)with single readout line!
26

Ds
be
to
of
se
he
on
eraon
nt
ti-

NWe
med
ate
m
to
r.
evel
m
or
he

noise spectrum is no longer white and noise
the noise
spectrumlevel isin no lonto the NbTiN
central line
1, inset)
and the NbTiN
increasesthe(Fig.
kinetic
inductancefractionincreasesby 45%theto kinetic
a ¼ 0.09inductance fraction by 45% to a ¼ 0.09
groundplane at the resonator short. The NbTiN is lossless forboth phase and amplitude readout is lower
both phasewith respect
and amplitud
andreducesthevolume
by
40%.
Both
and
give
reducesalineartheincreasevolume
by
40%.
Both
give
a
linearincreasefrequencies up to the gap 2D0 =h ¼ 1:1 THz ðTc ! 14 KÞ.
to P350GHz > 4 fW.
to P350GHz > 4 fW.
Any radiation
frequency
0:09 < ! < 1:1 THz is there- in the phase response.
inwiththeaphase
response.
10,11
10,11
fore absorbed in the Al (Tc ¼ 1.28 K) central line of the secFig.
2
shows
three
more
which
Fig.
may
2 shows
be present
three more
on
a
high
on a features,
high
An
array
of
24
pixelshas
beenfabricated
An
array
of
24
pixelshas
beenfabricatedond section. The optically excited quasiparticles are trappedin a photon noise
limited MKID.
in a photon
photon noise limited MK
resistivity
ð> 10tokXcmÞgaph100i-oriented
Si substrate.
ð> 10
AllkX
pixcmÞ h100i-oriented
Si substrate.
All pixin the Al because
it is connecteda highsuperconduc- resistivity
tor. This quantum
wellcapacitively
structure confinescoupled
the quasiparticles
in elsfeedline
photonnoise withlevela ofthe spectraTheobservedphotonin
Fig. levelels areto a single
are capacitively
with a coucoupled to The
a single
feedlinecoue-noise

Photon-noise limited NbTiN/Al hybrid MKIDs

2(a) is independentof the optical2(a) because
is independent
the prodof the op
QiQexpected
which
an is matchedto the Qi expected
for an loading
pling Qc " 58 k, which is matched to theplingc " 58 k,for-opticalNbTiN:
1.1
uctAfterofTHzquasiparticle
numberquasiparticle
uct
lifetime is connumber a
optical loading of "10 pW. After mounting
anloadingarrayFof
ofgap"10
16 =pW.
mounting anarray andof 16
Al of quasiparticle
and the loaded
Q Quantum-welldidstant,6,13
laser machined Si lenses with a diameter
laser machinedof 2 mm on
Si thelenses stant,with 6,13
a diameterof 2 mmon notthe change.
e- and the loaded Q di
6
- Lossless
spectrapresented
By fittinga Lorentzian
fittinga Lorentzian rcentral pixels, the array is evaluated using
centrala pulsepixels,tube
the prearray is evaluatedusing
a pulse(2Δ
tuberoll-off< prehν) to the By
in Fig. 2(a)we derive
thea quasiparticle
inlifetime
Fig. 2(a)as wea function
derive the qucooled adiabatic demagnetization refrigerator
cooled adiabaticwith a box-indemagnetization
refrigerator
withbox-in12
12-a-boxAl:
Farray90 GHzgap
ofIntheFig.
shows ofthatthetheopticalquasiparticle
loading. Fig.
thecold
is=fully
thisopticaldesignloading.
the arrayis 3fully
a-box cold stage design. In this design
stage
design.
lifetime obtainedphase andlifetime
readout
obtained
is equalfrom phase
enclosed in a 100 mK environment withenclosed
the exception
in a 100 ofmKa environment
with thefrom
exceptionof aamplitude- above
Quasiparticle
excitation
NbTiN
quasiparticle
forall15.05
loading
forfW
alltheloading
levels. For P35
2 mm aperture, which is located 15.05 mm
2 mm
aperture,
the approxiwhich is locatedmmlevels.
above For
the P
approxi350GHz > 100&0:5060:02&0:
Resonator/P
relation,whichmatches/P
lifetimes
a sqp
lifetimesshowasmate center of the MKID array. This aperturemate centeris isotropicallyof the MKID array.
Thisshow
apertureis isotropicallyqp
350GHz350
pﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃ 6
pﬃﬃﬃﬃﬃﬃﬃﬃ
13–15
6✴
Quasiparticle
Trapping
Al
(2Δ
>
hν)
/
1=
P
relationforahomoge/1=
P350
the expected sin
theexpectedsilluminated by a large temperature-controlled
illuminatedblackbody.
by a large
temperature-controlled
blackbody.
qp
350GHzqp
neously ailluminatedneously
P350GHz
illuminatedsuperco¼ 4 fW we
Two metal mesh filters provide a minimum
Two metalrejection
mesh filtersofprovideminimum superconductor.
rejection of At

FIG. 1. Scanning electron micrograph of the antenna-coupled hybrid
NbTiN-Al MKIDs used. A wide NbTiN CPW resonator is used to minimize
the two-level system noise contribution. At the shorted end where the planarantenna is located, one millimeter of CPW is reduced in width, and the central line is made from thin Al. The Al is galvanically connected to the
NbTiN at both ends (inset).

3, 203503-1

Photon noise PSD

NEP vs. P350 GHz

C 2013 AIP Publishing LLC
V

is subject to the terms at: http://scitation.aip.org/termsconditions. Downloaded to IP:: Thu, 05 Dec 2013 15:24:11

flat: photon noise

on
t
o
ph

se
i
no

lim

it

Relevant for
DESHIMA

AMKID camera array

Janssen et al., Appl. Phys. Lett. 103, 203503 (2013)
FIG. 2. (a) The power spectral density of the amplitude
FIG. 2. (dashed(a)
The powerline)
spectralphase(solidofthenoise
amplitude
measured(dashedunderline)
variousand opticalphase (solid
loading.
line)A noise
whitemeasured
noise specunder vari
Janssenet andal.,Appl.density
Phys.line)
Lett.
105,
193504(2014)> 100
The roll-off
abovepower,
1 kHz isto the>quasiparticle
100 fW. Thelifetime,roll-off which
above 1 kHz itrum is observed, the level of which is constant withtrumloading
is observed,
power,
theforlevel
P350GHzof which
is fW.
constant
with loading
fordue
P350GHzis reduced by an increasing optical load. Note thatis reduced
the photon
by an
noise
increasinglevel isoptical
16 dB higher
load. Notein phasethat thereadout.
photonNevertheless,noise level is
at 16
a givendB higherloading
in phase
the NEP
readout.
is the Neverth
27
6,7
6,7
amplitude(dashedline)(solidreadout
amplitude
as a function(dashed line)of opticaland phase (ssame for phase and amplitude readout as shown in
same(b).for(b)phase
The opticaland amplitude
NEP forreadout
as shownin (b).
(b)andThephase
optical
NEPline)for320-370 GHz filterbank chip(# this photograph is 1 generation older)

CPW line

Various test

(S=W=0.5µm)

resonators

MKIDs

Antenna

Filterbank(64 channels, F/ΔF = 500)

Cosmology with Nanotechnology

Contents
Introduction
Submm astronomy
DESHIMA
DESHIMA
On-chip Filterbank Spectrometer
MKID
Cryogenic System
OpticsReadout
Experimental Results
29Integration of DESHIMA

Google map
30

Cryogenic Optics: Cool Down Test
Configuration:• 4 K: Pulse tube cooler• 100 mK: ADR (2 stages)

Specification:• Hold time (w 1 uW loading) ~ 18hlog_2016-03-25 1657
0.8

FAA
Magnet current

0.7

Temperature [K]

0.6

0.5

0.4

hold time ~ 26h
w. 0.4 uW loading

0.3

0.2

0.1

0

14:00:00
27.03.2016

18:10:00
27.03.2016

22:20:00
27.03.2016

02:30:00
28.03.2016

06:40:00
28.03.2016

10:50:00
28.03.2016

15:00:00
28.03.2016

Time

31

Cryogenic Optics

4 K stage
field lensParabolic
Mirrorsheat switch
800 mK ‘finger’
100 mK ‘finger’
field lens
stray light baffle

300 K scatter filter (two-in-one)
50 K thermal filters
2 THz (66 cm-1) Low Pass Filter
4 K thermal filters

Nb shield

1.5 THz (58 cm-1) Low Pass Filter
1 .1 THz (36 cm-1) Low Pass Filter
polarizer

Cryoperm shieldfilterbank chip & lens
(at 100 mK)

1THz (33 cm-1) LPF + 390 GHz (13 cm-1) LPF(or 1THz (33 cm-1) LPF + 0.9THz (30 cm-1) LPF

32

Experiment at Delft
Re-assembled• Hold time (w. 0.4 uW loading) ~ 26h
Cool down with DESHIMA chip33

DESHIMA Readout System
Developed by SRON for SpaceKIDs project• J. van Rantwijk et al., IEEE TMTT, 64, 6, 1876-1883 (2016)

RF cabinet (RF board)

Computer

Digital cabinet (ADC/DAC board)DESHIMA Readout System
Developed by SRON for SpaceKIDs project• J. van Rantwijk et al., IEEE TMTT, 64, 6, 1876-1883 (2016)

Specifications:• FFT based readout• 2 GHz band width• Can read 4000 KIDs simultaneously• Maximum data rate ~1.3 kHz

35

Contents
Introduction
Submm astronomy and DESHIMADESHIMA
On-chip Filterbank Spectrometer
MKID
Cryogenic System
OpticsReadout
Experimental Results
36Measurement of frequency response
MKID sensor responds when FFilter = Fsignal

Fsignal response of different channels

VNA display

Frequency sweep with a photo-mixing CW source
Experimental setup

Cryo Optics
Into Cryo Optics
beam splitter

High power from InGaAs emitters
InGaAs-based terahertz emitters comprise ultrafast p-i-n photodiodes, with an intrinsic
layer embedded between p-doped and n-doped semiconductor layers. The laser lightis coupled into the intrinsic layer from an underlying waveguide structure. In this design,
the extended absorption length leads to highly-efficient terahertz generation.
InGaAs has a semiconductor bandgap of 1.68 μm and telecom lasers at 1.5 μm arethus a perfect match. The combination of ToPTIcA’s TeraBeam laser and InGaAs
emitter/detector modules presents a highly-compact terahertz platform, and achieves
power levels up to 10 μW.

High power from InGaAs emitters
InGaAs-based terahertz emitters comprise ultrafast p-i-n photodiodes, with an intrinsic
layer embedded between p-doped and n-doped semiconductor layers. The laser lightis coupled into the intrinsic layer from an underlying waveguide structure. In this design,
the extended absorption length leads to highly-efficient terahertz generation.
InGaAs has a semiconductor bandgap of 1.68 μm and telecom lasers at 1.5 μm arethus a perfect match. The combination of ToPTIcA’s TeraBeam laser and InGaAs
emitter/detector modules presents a highly-compact terahertz platform, and achieves
power levels up to 10 μW.

Specifications
Wavelength
Emitter
ReceiverAntenna type

Emitter / receiver bandwidth*

Specifications#EK-000685#EK-000724 / #EK-000725

GaAs

InGaAs on InP

Semiconductor material

1546 + 1550 nm

Wavelength

Photo-mixing
InGaAs THz Transmitter

Semiconductor material

853 + 855 nm#EK-000685
GaAs
853 + 855 nm

Photomixer

Waveguide-integrated
p-i-n photodiodeEmitter

Photomixer

Photomixer

Photomixer

ReceiverPhotomixer

Log-spiralBow-tie

Antenna typeLog-spiral> 3 Thz> 2 Thz

Emitter / receiver bandwidth*> 3 Thz

Photo-mixing
InGaAs THz Receiver(For reference)#EK-000724 / #EK-000725
InGaAs on InP

1546 + 1550 nm

Waveguide-integrated
p-i-n photodiodePhotomixer
Bow-tie> 2 Thz

Terahertz power (typ.)2 μW @ 100 Ghz
0.3 μW @ 500 Ghz

4 μW @ 100 Ghz
0.5 μW @ 500 Ghz

Terahertz power (typ.)2 μW @ 100 Ghz
0.3 μW @ 500 Ghz

Terahertz dynamic range(@ 300 ms integration time)

80 dB @ 100 Ghz
70 dB @ 500 Ghz

70 dB @ 100 Ghz
50 dB @ 500 Ghz

Terahertz dynamic range(@ 300 ms integration time)

80 dB @ 100 Ghz
70 dB @ 500 Ghz

70 dB @ 100 Ghz
50 dB @ 500 Ghz

cylindrical, Ø 1”,
integrated Si lens & SM/PM fiber pigtail

cylindrical, Ø 30 mm,
integrated Si lens & SM/PM fiber pigtail

cylindrical, Ø 1”,
integrated Si lens & SM/PM fiber pigtail

cylindrical, Ø 30 mm,
integrated Si lens & SM/PM fiber pigtail

Laser power < 50 mW
Bias ± 10 V

Laser power 20 mW
Bias 0 / -1.5 V

Package
Recommended operating
conditions
Key advantages

high bandwidth, high dynamic range

compact laser unit, low cost

Package
Recommended operating
conditions
Key advantages

4 μW @ 100 Ghz
0.5 μW @ 500 Ghz

Laser power < 50 mW
Bias ± 10 V

Laser power 20 mW
Bias 0 / -1.5 V

high bandwidth, high dynamic range

compact laser unit, low cost

* Tuning range of lasers may differ* Tuning range of lasers may differ

Filterbank chip at 100 mKorder information

order information
850 nm
#EK-000685

GaAs photomixer for cw terahertz generation and detection, with log-spiral antenna and
SM/PM fiber pigtail

850 nm
#EK-000685

GaAs photomixer for cw terahertz generation and detection, with log-spiral antenna and
SM/PM fiber pigtail

1550 nm#EK-000724

InGaAs/InP based waveguide-integrated photodiode for cw terahertz generation, withbow-tie antenna and SM/PM fiber pigtail

1550 nm#EK-000724

InGaAs/InP based waveguide-integrated photodiode for cw terahertz generation, withbow-tie antenna and SM/PM fiber pigtail#EK-000725

InGaAs/InP based photoconductor for cw terahertz detection,with bow-tie antenna and
SM/PM fiber pigtail#EK-000725

InGaAs/InP based photoconductor for cw terahertz detection,with bow-tie antenna and
SM/PM fiber pigtail

1.5 µm (200 THz) laser pair withdifference frequency ~350 GHz

note: The photomixers are available as individual modules or as part of the Spectroscopy extension (p. 25).
operation requires a set of seed lasers (e.g., the Standard Package SyST Thz STd / 850, or the TeraBeam 1550).

Delft
University ofTechnology

www.toptica.com | 23

note: The photomixers are available as individual modules or as part of the Spectroscopy extension (p. 25).
operation requires a set of seed lasers (e.g., the Standard Package SyST Thz STd / 850, or the TeraBeam 1550).

www.toptica.com | 23

37

Cosmology with Nanotechnolog
Cosmology

Spectroscopic responseFirst ‘usable’ on-chip filterbank spectrometeratmospherictransmission
at Atacama

38Frequency resolution (Q factor)

design: 500

39

Out-of-band rejection

40

Bring to ASTE in 2017

Bring to ASTE in 2017

Summary and Outlook- The submicron CPW process is capable of producing CPW filterswith F/ΔF = 500 at ~300 GHz.
- Successfully integrated the telescope instrument hardware for
DESHIMA- Can accelerate the R&D cycle to approach the following problems
towards a working filterbank chip that can be field-tested at ASTE:
1) High end-to-end coupling efficiency
2) Even frequency spacing throughout the band3) Good stray light rejection

First light of DESHIMA is expectedin autumn 2017 at the ASTE
Telescope !
43