2023年度光赤天連シンポジウム (2023/9/27-29)

ULTIMATE-Subaru
プロジェクト報告
https://ultimate.naoj.org/index.html

小山佑世 (国立天文台ハワイ観測所)

on behalf of ULTIMATE collaboration

Great synergy with future
space telescopes

Roman
EuclidJASMINE

Excellent target provider
for 30m -class telescopes

TMTGMTELTSF galaxy at z=2「地表層補償光学(GLAO)」を搭載し、広い視野(約20分角)にわたって星像改善を目指す① 8m級望遠鏡で最大視野のAO+近赤外撮像

Naturalseeing

GLAO② 宇宙望遠鏡に匹敵する解像度

GLAO (0.2”in K-band)③ ほぼ全天で実現

ガイド星条件r~19mag④ 多彩なフィルター群

naturalseeingプロジェクトチーム構成(1): 装置開発チーム・プロジェクトコアチーム
ULTIMATE-Subaru project office•••••••••••••••
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Michitoshi Yoshida (NAOJ, Project PI)
Yosuke Minowa (Subaru, Project Manager)
Yusei Koyama (Subaru, Project Scientist)
Takashi Hattori (Subaru, wide-field imager)
Yutaka Hayano (Subaru, GLAO development)
Junichi Katakura (Subaru, Project controller)
Kentaro Motohara (NAOJ, wide-field imager, WFI)
Hirofumi Okita (Subaru, Telescope upgrade)
Yoshito Ono (Subaru, GLAO development)
Ichi Tanaka (Subaru, MOIRCS upgrade lead)
Yoko Tanaka (Subaru, GLAO optical design)
Koki Terao (Subaru, GLAO development)
Chihiro Tokoku (NAOJ, NINJA development)
Shin Oya (NAOJ, GLAO development)
Kenshi Yanagisawa (NAOJ, System engineer, wide-field imager)
Hiroshige Yoshida (Subaru, GLAO/MOIRCS, software)
Sadman Ali (Subaru, sensitivity WG)
Masayuki Akiyama (Tohoku, GLAO development + science)
Tadayuki Kodama (Tohoku, Science team lead)
Hajime Ogane (Tohoku, GLAO/ULTIMATE-START)Masahiro Konishi (Univ. of Tokyo, wide-field imager)

ULTIMATE science core team
Akio Inoue (Waseda)•Tadayuki Kodama (Tohoku)•
Yusei Koyama (Subaru)•
Tomoko Suzuki (IPMU)•Ken-ichi Tadaki (NAOJ)•
Kosuke Kushibiki (Tokyo)•
Sakurako Okamoto (Subaru) ••
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Shogo Nishiyama (Miyagi Univ. Educ.)
Daisuke Suzuki (Osaka)
Takafumi Kamizuka (Tokyo)
Kumiko Morihana (Subaru)
Yuhei Takagi (Subaru)
Tsuyoshi Terai (Subaru)
Takashi Moriya (NAOJ)

ANU team (Australia)
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Celine d'Orgeville (ANU, team lead)
Doinne Haynes (ANU, project manager)
Noelia Martinez Rey (ANU, project scientist)
David Chandler (ANU, systems engineer)
Nicholas Herrald (ANU, mechanical engineer)
Israel Vaughn (ANU, Optical Engineer)
Warrick Schofield (ANU, Mechanical Engineer)

ASIAA team (Taiwan)
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Shiang-Yu Wang (ASIAA team lead, project management)
Masahiko Kimura (ASIAA, InR, Relay design)
Chueh-Yi Chou (ASIAA, Relay design)
Yin-Chang Chang (ASIAA, Relay design)Hsin-Yo Chen (ASIAA, InR design)プロジェクトチーム構成(2): サイエンスチーム

Science Goal (1): ULTIMATE for Deep Universe
Unveiling the life of galaxies across cosmic time and environment from elementary scale252) Growth of Galaxies

Deep & Wide NB

Sharp & Wide NB

Stellar build-up inside
the galaxies at thecosmic noon (z~2-3)epoch with deep andsharp NB(Ha/[OIII])imaging in K-band.

Unprecedentedly deepand wide NB imaging tosearch Lya emitters inthe epoch of cosmic
reionization (at z>>7)3) Death of Galaxies

H3
H1 H2

24

ULTIMATE-NBK

MAHALO-Deep

MAHALO-Subaru

23

CDFS(CFHT)HiZELS-HAWKIHiZELS-main

HiZELS-Deep

22

Bootes-HiZELS

21-2.0-1.5-1.0-0.50.0
2log (Survey Area) [deg ]4) Nearby Galaxies & Galactic SF Regions

Deep & Wide MB

Understand the nature and environment of massive(quenched) galaxies by detecting the most massive
galaxies at z~4-5 with deep/wide MB(K) imaging.

K1 K2

NB(K) [AB mag]

1) Birth of Galaxies

GOODS-S(HAWK-I)

K3
SEDs ofz=4
galaxySharp & Wide JHK+NB•

Spatially resolve nearby
galaxies (D<10Mpc) into stars
and star-forming regions.

•Sharp/deep imaging
of SF regions in theMilky Way to study theIMF.

0.5

Science Goal (2): ULTIMATE for Transient UniverseUnderstanding the evolution of stars, blackholes, and planets near and far
1) Galactic Center

3) High-z Supernovae

Sharp & Wide JHK + NB•

•High/low cadence survey
toward the Galactic Center withULTIMATE, to reveal hidden
objects (blackholes and freefloating planets) in the Galactic
Center with microlensing andastrometric approach.
Synergy with JASMINE, Roman.

2) Galactic Plane••

Deep K-band imaging•SNe search at z>6 – visiting ~1-deg2 every 180days down to K > 26 mag (AB) will allow us todetect PopIII pair-instability SNe at z>6.

•

Boost the SNe detectability by targeting
protoclusters/overdense regions identified by
HSC (and Euclid/Roman) survey.

SLSNe

PISNe

Sharp & Wide NB/MBRevealing the Milky Way
structure and hidden stellar
evolution (e.g. OH/IR stars).
Pab/Brg imaging for cataclysmic
variables, to reveal the Galactic
Diffuse X-ray Emission

Moriya+2019

Harikane+2019

ULTIMATE-Subaru – GLAO + WFI
2019年度より、国立天文台の「Aプロジェクト」として活動中
2028年のファーストライトを予定

ASM design

Optical/Mechanical design
Wide-fieldImager (WFI)

Prototyping
AdaptiveSecondaryLaser Guide StarFacility

Mechanical designOpticaldesign
Wavefront
SensorReal-time Controller+ Control system•••••Prototyping

RTC based on the CACAO
developed for SCExAO

科研費基盤S「すばる望遠鏡トモグラフィー補償光学で明かす銀河骨格の確立過程」(2017-2021年度, 代表: 秋山正幸)
科研費基盤S「高感度広帯域近赤外線分光で読み解く重力波源における元素合成」(2021-2025年度, 代表: 吉田道利)
科研費基盤B「JWSTと究極の多波長・高解像観測による銀河団銀河の形態発現プロセスの解明」 (2023-2025年度, 代表: 小山佑世)
研究拠点形成事業「地上・宇宙望遠鏡の連携による近赤外線広視野深宇宙探査時代の国際研究拠点形成」(2021-2025年度, 代表:吉田道利)
国際先導研究「宇宙における天体と構造の形成史の統一的理解」(2022-2028年度, 代表: 宮崎聡)

GLAO subsystem overview and status
Adaptive Secondary Mirror (ASM)••••

Φ=1260mm deformable mirror with 924 actuators
Adopt the well-developed technology from AdOptica/Italy.
Final design completed in FY2021
Fabrication started in FY2022

Laser Guide Star Facility (LGSF)

2022年11月にGLAOのPreliminary Design Review(PDR) を実施 à 合格

• Use 2 TOPTICA high-power lasers (22W) to generate 4 Laser Guide Stars.
• Launch the laser beams from the side of the telescope.
• Preliminary design ongoing.
Laser Beam(Φ~300mm)• ASM will be installed inthe existing Infrared
Secondary Mirror
mount

Wavefront Sensors (WFS)• Equip with the 4 LGS WFSs to measure the turbulence at theground layer and another 4 NGS WFSs to measure the low-ordererror that cannot be measured with the LGS.
• Preliminary Design completed in FY2021.

20 arcmin

Natural Guide Star (NGS) x 4Launching
Telescope

Key Technology Prototyping

TOPTICA
Laser Head

Diagnostics
Bench• ULTIMATE-START - a Laser Tomography AO (LTAO) Wavefront Sensor with 4 x SH-WFS - hasbeen developed for testing the camera, real-time control, etc. for the future GLAO system.
• TOPTICA laser guide star has been integrated at Subaru to provide 4 laser beams for LTAO.
• LTAO will be initially commissioned with AO188, and later be used with the ASM, providing
a narrow-field (<10”) LTAO mode in ULTIMATE.

Science FoV
14x14 arcmin2

LGS WFSNGS WFS
Laser Guide Star (LGS) x 4

TOPTICA laser commissioned at Subaru

LTAO WFS (ULTIMATE-START)GLAO Preliminary Design Review (Nov 2022)
審査員(アルファベット順)

Julia Bryant(Univ. of Sydney / Australia)• Mark Chun [Chair](Univ. of Hawaii / USA)
• Jerome Paufique(ESO)•oPhtdveoemRoHideki Takami(NAOJ / Japan)• Peter Wizinovich(Keck Observatory / USA)
• Takehiko Wada
(JAXA / Japan)•oPhtedv
moeoR

Expected GLAO performance
GLAO
naturalseeing

PSF uniformity(ΔPSF~10%
over the entire
14’x14’ FoV)
Minowa et al. (2020)

ULTIMATE-WFI (Wide-Field Imager)• 本体開発予算は大型科研費を申請中• MBフィルターの製作は国際先導研究で予算措置済

2021年に概念設計審査(CoDR) に合格
Lens Holding Overhang
5mm wide

226mm
216mm

15mm (0.52’)

CaF2
Field Lens

• Four-barrel optical design•

Motohara+2020

Field is divided into four parts with independent relay optics• 3 filter wheels to accommodate max. 15 filters per barrel• Accept many filters (BB, MB, NB)• Design for easy filter replacement during downtime

Unvignetted
FoV
7.2’ × 7.2’
(211 × 211mm)

Sensitivity – GLAO + WFI (broad-bands)
Point source sensitivity (5s, 1-hour) for ULTIMATE BB/MB/NB filters:• We can reach Ks = 25-26 mag (AB) with reasonable observing time.
• ~0.5 mag higher sensitivity than no-AO cases in K-band (~0.3-0.5 mag in Y/J/H).
理想的な条件

現実的な条件Sensitivity – GLAO + WFI (broad-bands)
Point source sensitivity (5s, 1-hour) for ULTIMATE BB/MB/NB filters:• We can reach Ks = 25-26 mag (AB) with reasonable observing time.
• ~0.5 mag higher sensitivity than no-AO cases in K-band (~0.3-0.5 mag in Y/J/H).
現実的な条件

理想的な条件
Roman
Ksバンド
感度

Roman Science and Technical Overview (ver. Summer 2023)

Sensitivity – GLAO + WFI (MBs/NBs)
Point source sensitivity (5s, 1-hour) for ULTIMATE BB/MB/NB filters:• We can reach Ks = 25-26 mag (AB) with reasonable observing time.
• ~0.5 mag higher sensitivity than no-AO cases in K-band (~0.3-0.5 mag in Y/J/H).
MBs

NBs

Only for best conditions – please expect ~0.3-0.5 mag shallower depths in the case of lower elevations.

研究拠点形成事業 2021年4月〜2026年3月, 代表: 吉田道利 (国立天文台)「地上・宇宙望遠鏡の連携による近赤外線広視野深宇宙探査時代の国際研究拠点形成」•••

2021〜2022年度にかけてオンラインセミナーを６回開催
2023年3月に対面ワークショップを開催
2024年度中に２回目のワークショップを開催予定

世話⼈: M.Yoshida/H. Miyatake/T. Moriya/D. Suzuki/Y.Koyama

REUPSULTIMATE “narrow-field (LTAO)” mode

Wide-field+ moderatecorrection• ULTIMATE is not only for wide-field science.
• Our “LTAO” mode can deliver ultimately highspatial resolution and high sensitivity for yourfavorite target! See O. Guyon’s talk fore more details
about narrow-field capabilities

Narrow-field+ diffraction limit

GLAO(~0.2“ @ K-band)
LTAO(~0.05“ @ all λ)Natural Seeing

LTAO© ESO (VLT/MUSE)NINJA

Near-INfrared and optical Joint
Spectrograph with Adaptive optics• LTAO対応, 高感度広帯域分光装置

ポスターもご参照ください(Tokoku et al.)

• 科研費(基盤S)による開発• 「高感度広帯域近赤外線分光で読み解く重力波源における元素合成」• 2021〜2025年度, 代表: 吉田道利 (国立天文台)• すばるのPIタイプ装置として提案予定 (2026年度運用開始を目標)

光学系
レイアウト

検出器上のエシェル
フォーマットNINJAメンバー: 東谷千比呂, 吉田道利, 守屋尭, 本原顕太郎, 尾崎忍夫, 柳澤顕史, 大野良人,美濃和陽典, 寺尾航暉, 早野裕, 小山佑世, 冨永望, 大内正己, 田中賢幸 (国立天文台), 田中雅臣,秋山正幸 (東北大学), 長尾透, 松岡良樹 (愛媛大学), 櫛引洸佑, 安田彩乃, 幸野友哉 (東京大学)

Tokoku et al. (2022)

Summary•

ULTIMATE = すばる２時代の明夜を担う次世代広視野補償光学 x 赤外線観測装置•

2017年度: ”ULTIMATE-START”始動 [科研費, 代表: 秋山正幸]•

2018年度: GLAOシステム Conceptual Design Review•

2019年度: 国立天文台Aプロジェクト (すばるGLAOプロジェクト)•2021年度: 本格的な予算措置スタート•

2021年度: SUPER-IRNET, NINJA始動 [科研費, 代表: 吉田道利]•

2021年度: 観測装置 Conceptual Design Review•

2022年度:「すばる２」始動, 可変副鏡の製作開始•

2022年度: GLAOシステム Preliminary Design Review•

2022年度: 国際先導研究スタート [科研費, 代表: 宮崎聡]

ファーストライト(2028年を予定)まであと５年！いよいよサーベイプランの検討が本格化するこのタイミングで、是非サイエンスチームにご参加ください。