ULTIMATE-Subaru
ULTIMATE-SUBARU
with Wide-Field Ground-Layer Adaptive Optics

Study Report - January 2016

Subaru Telescope
National Astronomical Observatory of Japan

美濃和陽典、小山佑世、(国立天文台ハワイ観測所）

ULTIMATE-Subaruワーキンググループ

光赤天連シンポジウム（2016.9.27)

すばるの次世代装置開発
2020年代にすばるが競争力を維持するためには？
Subaru Advisory Committeeからの提言（2009)

1. Very wide-field optical imager

SupCam ̶> HSC (2013)

2.Wide-field multi-objet spectrograph

FOCAS, FMOS ̶> PFS (2019)

3.Wide-field near-infrared imager and multi-object (IFU) spectrographDark1nights

Bright1nights

IRCS, MOIRCS	

̶> ULTIMATE (2023)

PFS
ULTIMATE

HSC
1λ"[um]2

すばるの次世代装置開発：近赤外線
地表層補償光学 x 広視野近赤外線装置
89

GLAOによる星像改善シミュレーション
GLAO performance simulation

On-sky performance with RAVEN

Figure 6.3: Left: Improvement of the seeing probability distribution (dotted line) to GLAO performanceprobability distribution (red line). The error bars are the standard deviation along the time axis. Right:
confirmation of simulation results by Raven used in GLAO mode: the white star shows the result of nocorrection while the green star is the result of RAVEN.
Result of MOAO performance simulationFigure 6.3: Left: Improvement of the seeing
distr(Oyaprobabilityet al. 2014)
probability distribution (red line). The error bars are the sta
confirmation of simulation results by Raven used in GLAO
correction while the green star is the result of RAVEN.

視野20分角超にわたって一様にシーイングを向上させる

We plot the wavefront error in Fig. 6.7. Total wavefront error is shown in filled square. Cross mark showsa tip-tilt wavefront error from natural guide star and open square shows a high-order wavefront error
from laser guide star. Plots from upper left to lower right correspond the guide star constellation, whichis shown in Figure 6.6 from left to right. The horizontal axis shows a distance from the center of field ofview, which starts from the bottom to the top of the guide star constellation shown in Figure 6.6. Three
natural guide stars lies at the vertical dash line in triangle, and five laser guide stars at the vertical doted
line in pentagon. The horizontal lines at the wavefront error of 350nm and 240nm are equivalent to theStrehl Ratio of 0.4 and 0.2 at K band, respectively. The wavefront error become minimum at the center

Result of MOAO performance simulationULTIMATE-Subaru: 装置概要
(3)波面センサー x 8(1) 可変副鏡

カセグレン焦点φ~16arcmin

Microgate ADS

広視野近赤外線装置(4)広視野近赤外線撮像装置• 撮像• 多天体分光• 多天体面分光(2) レーザーガイド星 x 4
TOPICA ファイバーレーザー(589nm) x 2

ULTIMATE-Subaru: 視野比較

FoV(comparison(of(NIR(facilities(in(2020年代の近赤外線装置との視野比較
2020s(available(at(λ>~2um(Subaru/MOIRCS((4’(x(7’)

Subaru/IRCS((1’x1’)

HST/WFC3((2.0’x2.3’)

VLT/HAWK:I((7.5’(x(7.5’)ULTIMATE:Subaru((16’(x(16’)

JWST/NIRCAM((2(x(2.2’(x(2.2’)

ULTIMATE-Subaru:
性能予測
ULTIMATE(SUBARU(–(GLAO(Expected(Performances(VLT((Le(Louarn(and(al.)(:(Seeing(0.8’’(N>(GLAO(0.4’’(K(–(7.5’(FoV(Simulation by S. Oya

GLAOの基本仕様

ULTIMATE(SUBARU(–(New(AO(system(overview(((LGSNGSULTIMATE-AOで必要なガイド星の配置
20ʼ

ULTIMATE-Subaruで必要な望遠鏡改修(1) 16分角超の視野を確保するためのカセグレン改修• ADC, AG, Cal, SVをカセグレ
FoV~16ʼ

ン焦点から撤去(<10% vignet)• 既存カセグレン装置が使用できなくなる(2)赤外副鏡の改修

104

Figure6.14:
6.14: Unvignetted
Unvignetted FoVFoV atat Cassegrain
Cassegrain focus.
FigureFigure 6.14: Unvignetted FoV at Cassegrain• 可変副鏡を既存の赤外副鏡ユニットにインストール• Tip/Tilt機能を失う• 改修期間中1~2年程度赤外副鏡を使用できなくなる

re 6.22: Subaru ASM and available space in the existing IR secondary mirror

主鏡再蒸着期間を利用しダウンタイムを最大限に減らす

可変副鏡による多様なすばるの性能向上
TMT第1期装置がカバーしない装置仕様をすばる＋可変副鏡で実現

•

•

-

高分散分光（ R>100,000)-

熱赤外線観測 (> 3.0 ミクロン)-

極限補償光学（Extreme AO)

Single Conjugate AO (SCAO)による熱赤外線観測の性能向上-ストレール比 ~ 1.0 (> 3.0ミクロン)-

熱背景放射を増やすことなく、既存赤外線装置(IRCS, COMICS）の性能を大幅に向上

レーザートモグラフィー AO (LTAO) による可視域 (< 1.0 micron)の性能向上-•}

ストレール比> 0.5 at 0.7 micron

Adaptive Optics for Extremely Large Telescopes II: Esp
system on-sky results

In the left side of Figure 3, the measured SR values are reportevalue. A rectangle identifies points measured with seeing value
The scatter of the SRs values is large and goes from 80% to 15%
reports the considered values plotted against the tip-tilt (TT) pow~13 Hz. The correlation between SRs and vibration power isvibration is related to the LBT telescope structure and in particu
support the secondary and the tertiary mirrors. The LBT Observ
reduce the amplitude of these vibrations. The vibrations are noforce mostly depending on the ground-layer wind speed and its
line of sight of the telescope. It has been clearly seen during th
off-wind delivers better performance than looking straight inparticular when the sampling frequency of the system is less than

3.3. The achieved PSF contrast

One important result achieved with the LBT FLAO system is thecorrected images, which is very important to detected faint poinrequired in searching for extra-solar planets. Figure 4 shows
AO-assisted high-dispersion spectrograph (R~160,000) at 0.35-0.9 micron with HDS corrected PSF in H band taken on June 25th 2010. Several imand non-saturated) to compute the PSF profile with the required
magnitude of the GS (HD175658) is 6.5 and the estimated see
AO-assisted visible IFU spectroscopy with FOCAS or Kyoto-3DII
data oscillated between 0.6 and 0.8 arcsec. The AO loop was run
KL modes. Some residual TT vibrations @ 13.0-13.7Hz of 6 toestimated SR in H band is >80%.

極限補償光学(ExAO)による可視〜近赤外線(0.6-2.5ミクロン)の観測性能向上-

既存のSubaru Coronagraphic Extreme AO (SCExAO)の性能、透過率（感度）向上-

可視〜近赤外線で高コントラスト観測を実現

Hバンド
ストレール比~0.8
LBT可変副鏡

Figure 4 (Left) The high order corrected LBT PSF in H band. Severa7.2.1

Four barrel imager design (J. Pazder, HIA)

Here we summarize a conceptual study by John Pazder (NRC-NSI-AST/HIA) based on his technicalnote ”Subaru concentric corrector and four barrel GLAO imager Optical Design Concept” (5/29/2013).
Because the available field-of-view at Subaru Cassegrain focus was still under study at the time when
his technical note was written, ∼ φ20′ is assumed in this study.
The concentric corrector consists of two elements of Infrasil-302 with spherical surfaces and 690mm
n diameter. It provides a universal 22′ .8 diameter field of view (at f/12.4) with residual optical design
aberrations less than 66mas. This corrector is designed to feed multi-barrel optical systems without pupil
miss-match.
The imager design concept is a four-barrel imaging system feed by this corrector with each barrel
having a 4k×4k H4RG detector covering a 6′ .8 × 6′ .8 field of view (0′′ .1/pixel sampling). The total
mager field of view is 185 square arc minutes.
Figure 7.1 shows the optical layout of this system. The cameras are within a volume of 2.1 m in lengthand 0.8 m in diameter. A window has been put at the entrance to the cameras, with the intention of thecameras being enclosed in the Dewar with the corrector and wave front sensors outside the Dewar. Thecameras have been designed with a sharp pupil image.

Spatial sampling per element
0.15 arcsec
Total field of view per IFU
1.18 square arcsec
Total patrol areaφ ∼ 15 arcminb
Minimum separation between IFUs 25 arcsec
Spectrograph (MOIRCS)
Wavelength coverage
0.9-1.8 µm
Spectral resolving power
500-3000
Dispersion
1.6 Å per pix (J), 2.1 Å per pix (H)Sampling
2-5 pixels in FWHM
Combined properties
fibres (fiducials) on each Starbug, as shown in Figure 7.19.
fibres.(H)
Additionally
there are a number (∼ 16)
Designby Australian AstronomicalObservatory
Total
eﬃciency
9% metrology(J), 12%ULTIMATE-Subaru: 近赤外線装置コンセプト
撮像装置

Design by HIA, Canada (J. Pazder et al.)

多天体面分光装置

plate. Thus, fine positioning is then achieved while the telefiducials
to thespectrograph.
field-plate fiducials. Acquisition is thenThis number can be increased by using a newlarger
stars.The
positional
accuracy of Starbugs is better than 5 mb
FoV of the wide field corrector.
on sky, and typical reconfiguration times are achievable wita(S. Ellis et al.)Starbugファイバーポジショナー• 最優先に開発を進めるを使ったファイバーIFU• 多様な狭帯域フィルターを搭載• チューナブルフィルターも検討• 国際協力による開発も検討

Figure 7.19: (Left) Starbugs on a field-plate, showing theslippers. (Right) Schematic view of the Starbug, showing theport and wires access ports on the backside. The Starbug
shares much of the technology with the TAIPAN system
and will be demonstrated its on-sky feasibility in early 201

多天体スリット分光装置

Figure 7.1: Optical layout of the corrector and imager system (J. Pazder, section 7.2.1)

The image quality is shown in Figure 7.2. Spot quality is less than pixels at all points except at theoutside corner where the image quality is marginally more at 16 µm RMS spot diameter.
116• MOIRCSを再利用• ナスミスに移設• 性能向上と安定化

The Starbug fiber positioner is a new technology devel
the TAIPAN instrument at the UK Schmidt telescope. TA
comprehensive spectroscopic survey and to prove the concep
to use on the Giant Magellan Telescope. TAIPAN will starstrate the feasibility of the Starbug technology, reducing thThe ULTIMATE Starbugs diﬀer from the TAIPAN Starbu
a heavier payload, and will operate at a lower atmospheri
to adhere the Starbugs to the field-plate and allow norma
Starbugs for the ULTIMATE instrument.

• オーストラリアとの国際協力による開発に期待
Integral field unit
• AAOによる概念設計

The IFU unit consists of three main components, the foreThese components are aligned and glued into position in a
into the Starbug.
The fore-optics magnify the beam from the telescope tlenslet array (magnification is about 3.5 to have a lenslet
lenslet). In principle, one could place the lenslet array dirusing the fore optics. However, there are advantages to a lara large lenslet size compared to the fibre core diameter min
focal ratio degradation (FRD). Secondly, small lenslets areare likely to be expensive and to pose a significant risk in m
significant experience working with larger lenslets, having us
the use of fore-optics has advantages other than its eﬀectKey Science Case

広視野・高解像度・高感度ナローバンド
サーベイで切り拓く超深宇宙探査• Lyα輝線 (z=8,9,10,…)を用いた初代銀河の検出• Hα/[OIII]輝線を用いた銀河形成ピー
ク期(z=1-3)の小質量「ビルディング・ブロック」探査と空間分解• HSC(+PFS)による輝線銀河探査の長波長側への直接の拡張• HST/WFIRSTと同レベルの空間解像度＋JWSTを凌ぐサーベイ能力• TMTへのターゲット供給

with%GLAO%(0.2”)

seeingz=8.7
z=11.8z=7.7 z=10.0

Key Science CaseULTIMATE(K*: 究極のKバンド探査• 系内・系外サイエンスを問わず、広視野Kバンドサーベイを必要とする全てのサイエンスに威力• 例:「初代楕円銀河」の探査 ＠ z~5• 既存のUKIDSS-UDSなどよりも１等以上深く、１桁以上広いサーベイを実現。
• WFIRSTとの長波長側でのシナジー(明夜での貢献)の可能性
Galaxy spectraat z=4WFIRSTULTIMATE-K

Ultra&deep**
J*&*H**

HSC*(optical)**&*ULTIMATE&K*

Key Science Case
多天体面分光サーベイによる
銀河解剖とハッブル系列の起源

Comparison of ULTIMATE to existing and planned integral field spectrogr• SAMI/MaNGA等と同じ物理解像度でハッブル系列の形成期(z>1)に遡って銀河３次元分光探査を行う。
• オーストラリアとの国際協力。TMT時代を前に、我が国のコミュニティが面分光サイエンスの経験を積むきっかけになることを期待。

ULTIMATE-Subaru Study Report 2016
http://www.naoj.org/Projects/newdev/ngao/20160113/ULTIMATE-SUBARU̲SR20160113.pdf• Science Case
• Adaptive Optics• Instruments• Development Plan

外部評価委員によるレビュー

ULTIMATE-SUBARU 評価委員: 吉田(広島大、Chair), 土居（東大）, 嶋作（東大),with Wide-Field Ground-Layer Adaptive Optics
Kissler-Patig (Gemini), Renzini (INAF)
Study Report - January 2016

Subaru Telescope
National Astronomical Observatory of Japan

レビューアーからの提言•

競争相手となる装置（VLT/GRAAL+HAWK-Iなど）と比べて遅れて立ち上がるが、それでもユニークなサイエンスケースが必要。

•

開発コスト（50億円超）が膨大であるため、開発の優先度を決めて、段階を踏んだ開発計画が必要（まずはGLAO）。

•

撮像装置でのサイエンスが最もユニーク。撮像装置を優先すべき•

多天体分光などその他の装置については既存装置の再利用を検討。

ULTIMATE Subaru: スケジュール
NAOJ investment for PFS
CY

2016

2017

Concept Design

2018

2019

Prelim. Design

2020

2021

2022

2023

Detail Design
ASM Fabrication
Telescope Mod.

GLAO
AO experiment / Fibre Laser

WFS / GLAO development
AIT

WFI

Concept Design

Prelim. Design

Detail Design

Fabrication
AIT

Concept / Prototype

M-IFS

DesignFabricationAIT / Eng w/MOIRCS
Phase 2 Design

Science w/o GLAO

Phase 2 Fabrication

Next mile stone: Conceptual Design Review (including feasibilitystudy) for GLAO and WFI at the end of FY2017→開発コスト
Items

Cost (USD)

Budget(1) ASM system$6M(2) Laser system$1-4M(3) WFS unit

$3.5M

JSPS Grant-in-aid(4) Real time system$0.2M

JSPS Grant-in-aid(5) Telescope modiﬁcation$10M

NAOJ operation budget
as a part of Telescope upgrade(6) NIR instruments$5-15M

JSPS grant-in-aid & International collaboration(7) Human resources$2MNAOJ operation & JSPS Grant-in-aid(8) Contingency$5M

NAOJ operation budget

Total$40-50M

NAOJ operation budget
as a part of Telescope upgrade
JSPS Grant-in-aid(Partly purchased by NAOJ budget for AO188)(2), (3), (4): 科研費による予算獲得を目指す(6): まずは撮像装置の予算獲得を目指す。国際協力による開発推進に期待国際共同運用との関連性•ULTIMATEはHSC,	  PFSと同様に国際協力で開発を進めることを検討	  -­‐ NAOJ単体での開発はほぼ不可能、開発コスト、開発人員の分担を期待	  •ULTIMATEはすばるの次期facility装置であり、開発に参加することはすばるの機能向上につながる	  -­‐ ULTIMATE-­‐Subaruの開発への参加を国際共同運用への寄与とみなすことを検討	  -­‐ ULTIMATE-­‐Subaruが次期facility装置としてコミュニテイの認知を得ることが必要	  •国際共同運用の観点で、オーストラリアがULTIMATEの開発、サイエンス検討への参加に興味	  -­‐ すでにULTIMATE-­‐Suabruの多天体面分光装置の検討で協力	  -­‐ まずはULTIMATEに関連したいくつかの小規模のプロジェクトでの協力体制を築くことを進める	  ✴すばるAOのレーザーアップグレード	  (Celine	  D’Orgeville	  at	  ANU)	  ✴GLAO,	  LTAOの性能シミュレーションによる装置仕様検討	  (Francois	  Rigaut	  at	  ANU)	  ✴多天体面分光装置の概念設計とプロトタイピング（Andy	  Sheinis	  and	  Simon	  Ellis	  at	  AAO)	  ✴撮像、多天体面分光装置でのサイエンス検討での協力	  (Chris	  Lidman	  at	  AAO)	  •オーストラリアだけではなく、装置開発の面でカナダ、台湾からの協力に期待

まとめ•	  2020年代にすばるの「明夜」の競争力を維持するためには、近赤外線の新装置開発が不可欠	  •HSC,	  PFSに続くすばるの広視野戦略としてGLAO+近赤外線装置で大規模近赤外線サーベイを行うULTIMATE-­‐Subaru計画を推進	  •2017年度末のConceptual	  Design	  Reviewに向けて検討中	  -­‐ GLAOと撮像装置のfeasibility	  studyから始める	  •	  ULTIMATE-­‐Subaruの開発への参加をすばるの国際共同運用への寄与とすることを検討	  -­‐ まずはオーストラリアとAO開発の協力体制を築くところから始つつある	  -­‐ 観測装置の開発については、オーストラリア、カナダ、台湾との協力へ期待	  •ULTIMATE-­‐Subaruはすばるの次期Facility装置であり、日本のコミュニティの理解と協力が必須	  -­‐ ULTIMATE-­‐Subaruのサイエンス検討、装置仕様検討への「日本のコミュニティ」の参加を求む！	  
-­‐ 日本のコミュニティの意見を元に装置仕様を構築していくべき	  -­‐ 今が装置仕様に意見を反映させる絶好のタイミングULTIMATE-Subaruの検討にご関心のある方は是非ご連絡ください