The first light at ASTE
ALMA/45m/ASTE Users Meeting 2017
Kenichi Karatsu (SRON)

12Collaboration
Akira Endo, David Thoen, Ozan Yurduseven,Sjoerd Bosma, Nuria Llombart, Teun Klapwijk

Kenichi Karatsu, Robert Huiting, Vignesh Murugesan,
Stephen Yates, Jochem Baselmans

Tsuyoshi Ishida, Akio Taniguchi,
Tatsuya Takekoshi, Kotaro Kohno

Tai Oshima, Shun Ishii, Kahwuy Chin, Jun Maekawa,
Ryohei Kawabe, Toshihiko Kobiki, Shinichiro Asayama
Masato Naruse

Koyo Suzuki, Tetsutaro Ueda, Yoichi Tamura
Kazuyuki Fujita, Akira Kouchi

Paul van der Werf

Shunichi Nakatsubo

Tom Bakx2

3

Deep Spectroscopic High-redshift Mapper3

Deep Spectroscopic High-redshift Mapper

長崎 出島 / 出嶋

3

Deep Spectroscopic High-redshift Mapper

2D projection

長崎 出島 / 出嶋

Galaxies in
3D space

Imaging camera → 2D projection
The 3rd dimension = distance (time)

Goal: 3D map of massive starforming galaxies (Bright in the THz)distance (time)3

Idea:
On-chip Filterbank+ Microwave Kinetic Inductance Detector (MKID)DESHIMA [CII] survey
z = 1.6 - 6.9
Filter:Signal Frequency

widebandsignal720 718.6 717.1
GHz GHz GHz

leaky-lensantenna

6.000
5.996
GHz5.992
GHzGHzNbTiN
Al

241.0 240.5 240
GHz GHz GHz~500
channels(lens in behind)

Microwave Readout(4-6 GHz)

MKID:
ReadoutFrequency(absorber)

4.008
GHz 4.0044.000
GHzGHzNo metal

4

Breakthrough for 3D View of the THz Universe:
The effect of FIR lines on the selection of high-z galaxies

L97

Smail et al., Figure
2011 3. The contribution as a function of the source redshift to the continFigure 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-linecontributions. 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 aroundthe dust peak, with a linear flux scaling). We also indicate the observedframe passbands for the Herschel PACS (160 µm) and SPIRE (250, 350 andALMA (8 GHz)uum emission in the Herschel PACS and SPIRE, SCUBA-2 and LABOCA
bands, from the emission lines shown in Fig. 2. The influence of the[C II] 158 µm line can be seen in the 250-, 350-, 500- and 850-µm bands atz ∼ 0.6, 1.2, 2.2 and 4.4, respectively, with a contribution to the broad-band
fluxes of 5–10 per cent. Note that these contributions are based on a [C II]line comprising 0.27 per cent of the galaxy’s LFIR . The line contributions
will scale linearly with the line-to-FIR luminosity ratio, so sources with
L[C II] /LFIR ! 1 per cent (Fig. 1) will have contributions greater than orequal to four times larger, ∼20–40 per cent, corresponding to the right-handflux scale. We caution that the contributions for the higher redshift sourcesin the shorter wavelength filters (e.g. at z ∼ 4 and z ∼ 6 at 250 and 350 µm,respectively) are based on predicted, rather than observed, line fluxes.

5Breakthrough for 3D View of the THz Universe:
Wideband spectrometer
The effect of FIR lines on the selection of high-z galaxies（DESHIMA）

L97

Smail et al., Figure
2011 3. The contribution as a function of the source redshift to the continFigure 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-linecontributions. 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 aroundthe dust peak, with a linear flux scaling). We also indicate the observedframe passbands for the Herschel PACS (160 µm) and SPIRE (250, 350 andALMA (8 GHz)

(480 GHz)uum emission in the Herschel PACS and SPIRE, SCUBA-2 and LABOCA
bands, from the emission lines shown in Fig. 2. The influence of the[C II] 158 µm line can be seen in the 250-, 350-, 500- and 850-µm bands atz ∼ 0.6, 1.2, 2.2 and 4.4, respectively, with a contribution to the broad-band
fluxes of 5–10 per cent. Note that these contributions are based on a [C II]line comprising 0.27 per cent of the galaxy’s LFIR . The line contributions
will scale linearly with the line-to-FIR luminosity ratio, so sources withL[C II] /LFIR ! 1 per cent (Fig. 1) will have contributions greater than orequal to four times larger, ∼20–40 per cent, corresponding to the right-handflux scale. We caution that the contributions for the higher redshift sourcesin the shorter wavelength filters (e.g. at z ∼ 4 and z ∼ 6 at 250 and 350 µm,respectively) are based on predicted, rather than observed, line fluxes.

5Breakthrough for 3D View of the THz Universe:
40 cm

Wideband spectrometer
The effect of FIR lines on the selection of high-z galaxies L97（DESHIMA）
optical grating(ZEUS-2)

2 cm

Smail et al., Figure
2011 3. The contribution as a function of the source redshift to the continFigure 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 ofthe 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 aroundthe dust peak, with a linear flux scaling). We also indicate the observedframe passbands for the Herschel PACS (160 µm) and SPIRE (250, 350 andALMA (8 GHz)

(480 GHz)

on-chip filterbank(DESHIMA)

uum emission in the Herschel PACS and SPIRE, SCUBA-2 and LABOCA
bands, from the emission lines shown in Fig. 2. The influence of the[C II] 158 µm line can be seen in the 250-, 350-, 500- and 850-µm bands atz ∼ 0.6, 1.2, 2.2 and 4.4, respectively, with a contribution to the broad-band
fluxes of 5–10 per cent. Note that these contributions are based on a [C II]line comprising 0.27 per cent of the galaxy’s LFIR . The line contributions
will scale linearly with the line-to-FIR luminosity ratio, so sources withL[C II] /LFIR ! 1 per cent (Fig. 1) will have contributions greater than orequal to four times larger, ∼20–40 per cent, corresponding to the right-handflux scale. We caution that the contributions for the higher redshift sourcesin the shorter wavelength filters (e.g. at z ∼ 4 and z ∼ 6 at 250 and 350 µm,respectively) are based on predicted, rather than observed, line fluxes.

10 cm

40 mm x 15 mm
5330-370 GHz filterbank chip
CPW line

Various test

(S=W=2µm)

resonators

40 mm
15 mm

Antenna

MKIDs

Filterbank(49 channels, F/ΔF = 350)

Cosmology with Nanotechnology

Measurement of frequency response at LabNiTbNlA
latem oN

omed siht ni desu pihc knabretlfi eht fo citamehc

Frequency sweep with a photo-mixing CW source

yldetaeper si ycneuqerf ecruoSegnar siht dnuora gnitallicso

Sourceslennahwindow
c tnereffid fbeamo esnopsplitter
ser langisF

putes lscitpO oyrC

- F/ΔF = 300 ± 50
- 100 % yield rate (49/49)

rev

Km 001 ta pihc knabretliF

7

Aim of the 2017 engineering campaign❖

Baseline goal•❖

Test end-to-end operation of the DESHIMA system on ASTE, and confirm that weunderstand everything consistently between the lab and on ASTE.
•Interface checks•

Characterization of KIDs on ASTE

•Identify problems that can be found only by an actual installation, and not in thelab.

-If there are no critical problems, then we can leave the DESHIMA cryostat atASTE, so that future upgrades can be made with only exchange of chips.

•In practical terms:•

Full success: we are able to see continuum emission from a planet, weunderstand the response, and the cryostat can stay in Chile•

Success: we are able to learn new lessons by operating KIDs in the ASTE
cabin, either with or without signal from the sky.

•Failure: we learn only problems that we could have addressed and solved inthe lab.

Bonus goal

Slide From DESHIMA
Review in June 2017

•Detection of an astronomical line signal using an on-chip filterbank.

-If successful, this will be the first-light for a filterbank technology by any group.

Cosmology with Nanotechnology

The first campaign at ASTE: Oct. - Nov. 2017

9

The first campaign at ASTE: Oct. - Nov. 20179

10

https://www.youtube.com/watch?v=3ty3EgtQ_6g
or10

DESHIMA First Light !

11

DESHIMAFirstDESHIMA/ASTE
1stLightlight! !
357 GHz channel• 2017/10/19 19:10 (UTC)(16:10 CLST)• Source: Saturn

12CO (3-2)

HCN
HCO+a.u.

er
PyreVyranilim

Ori-KLNGC253
CO (3-2)
Contour: 2.5, 3.5, 4.5 … 9.5 σ
11Aim of the 2017 engineering campaign❖Baseline goal•❖

Test end-to-end operation of the DESHIMA system on ASTE, and confirm that weunderstand everything consistently between the lab and on ASTE.
•Interface checks•

Characterization of KIDs on ASTE•

Identify problems that can be found only by an actual installation, and not in thelab.

-If there are no critical problems, then we can leave the DESHIMA cryostat atASTE, so that future upgrades can be made with only exchange of chips.

•In practical terms:•Full success: we are able to see continuum emission from a planet, weunderstand the response, and the cryostat can stay in Chile•

Success: we are able to learn new lessons by operating KIDs in the ASTE
cabin, either with or without signal from the sky.

•Failure: we learn only problems that we could have addressed and solved inthe lab.

Bonus goal

Slide From DESHIMA
Review in June 2017•

Detection of an astronomical line signal using an on-chip filterbank.

-If successful, this will be the first-light for a filterbank technology by any group.

Cosmology with Nanotechnology

Aim of the 2017 engineering campaign
goalgoal✔ Baseline
Baseline❖•

Test end-to-end operation of the DESHIMA system on ASTE, and confirm that weunderstand everything consistently between the lab and on ASTE.
•Interface checks•

Characterization of KIDs on ASTE•

Identify problems that can be found only by an actual installation, and not in thelab.

-If there are no critical problems, then we can leave the DESHIMA cryostat atASTE, so that future upgrades can be made with only exchange of chips.

•In practical terms:•Full success: we are able to see continuum emission from a planet, weunderstand the response, and the cryostat can stay in Chile•

Success: we are able to learn new lessons by operating KIDs in the ASTE
cabin, either with or without signal from the sky.

•Failure: we learn only problems that we could have addressed and solved inthe lab.

goal✔ Bonus
Bonus
goal

❖

Slide From DESHIMA
Review in June 2017

•Detection of an astronomical line signal using an on-chip filterbank.

-If successful, this will be the first-light for a filterbank technology by any group.

Cosmology with Nanotechnology

Summary & Prospective
DESHIMA specs
2017

Goal (2019?)

frequency

330-370 GHz

240-720 GHz

F/ΔF

350

500

# of pixels

13?

NKID

50max 4000

13

Summary & Prospective
DESHIMA specs
2017

Goal (2019?)

frequency

330-370 GHz

240-720 GHz

F/ΔF

350

500

# of pixels

13?

NKID

50max 4000

13

Summary & Prospective
DESHIMA specs
2017

Goal (2019?)

frequency

330-370 GHz

240-720 GHz

F/ΔF

350500# of pixels

13?

NKID

50max 4000

Successful DESHIMA 1st Campaign at ASTE:
Oct. - Nov. in 2017
First-light for superconducting on-chipfilterbank technology in human history
Full spec. DESHIMA is under development for
the next campaign
For more results, please see poster by Koyo
Suzuki13

Summary & Prospective
DESHIMA specs
2017

Goal (2019?)

frequency

330-370 GHz

240-720 GHz

F/ΔF

350500# of pixels

13?

NKID

50max 4000

Successful DESHIMA 1st Campaign at ASTE:
Oct. - Nov. in 2017
First-light for superconducting on-chipfilterbank technology in human history
Full spec. DESHIMA is under development for
the next campaign
For more results, please see poster by Koyo
SuzukiThank you so much for lots of supports fromNAOJ Chile Observatory

13

Summary & Prospective
DESHIMA specs
2017

Goal (2019?)

frequency

330-370 GHz

240-720 GHz

F/ΔF

350

500

# of pixels

13?

NKID

50max 4000

Successful DESHIMA 1st Campaign at ASTE:
Oct. - Nov. in 2017
First-light for superconducting on-chipfilterbank technology in human history
Full spec. DESHIMA is under development for
the next campaign
For more results, please see poster by KoyoSuzuki
Thank you so much for lots of supports fromNAOJ Chile Observatory

Don’t forget to check the youtube movie!
13https://www.youtube.com/watch?v=3ty3EgtQ_6g
or14