ULTIMATE-Subaru \ ULTIMATE-SUBARU PROJECT OVERVIEW SUBARU - - PowerPoint PPT Presentation

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ULTIMATE-Subaru \ ULTIMATE-SUBARU PROJECT OVERVIEW SUBARU - - PowerPoint PPT Presentation

Jan 05, 2023 190 likes •445 views

() ULTIMATE-Subaru Christophe Clergeon,

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SLIDE 1

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

吉田道利、岩田生、大野良人、服部尭、Christophe Clergeon, 三枝悦子、沖田博文、田中壱、 高遠徳尚、有本信雄（ハワイ観測所） 早野裕、大屋真、高見英樹（国立天文台） 秋山正幸、児玉忠恭（東北大） 本原顕太郎、小西真広（東京大） Francois Rigaut, Celine D’orgeville, Gaston Gausachs, Nick Herrald, Visa Korkiakoski (ANU) Shiang-Yu Wang, Chi-Yi Chou (ASIAA)

ULTIMATE-Subaru

プロジェクトの概要

\

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SLIDE 2

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT OVERVIEW

SUBARU STRATEGIC PLAN TOWARD 2020 AND BEYOND

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Recommendation from Subaru Science Advisory Committee

1. Very wide-field optical imager

  • 2. Wide-field multi-objet spectrograph
  • 3. Wide-field NIR imager and MOS/IFU spectrograph w/ AO

HSC (2013) PFS (~2021) ULTIMATE(~2026)

HSC

PFS ULTIMATE

λ [um]

Img. Spec.

1 2 Dark nights Bright nights (2013-) (~2021-)

(~2026-)

ULTIMATE = ULTRA-WIDE-FIELD LASER TOMOGRAPHIC IMAGER and MOS with AO for TRANSCENDENT EXPLORATION by SUBARU

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SLIDE 3

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT STATUS REPORT

WIDE-FIELD ADAPTIVE OPTICS: GLAO

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https://www.eso.org/sci/facilities/develop/ao/ao_modes/.html

  • Turbulence profile at MaunaKea
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SLIDE 4

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT STATUS REPORT

ULTIMATE-SUBARU GLAO SYSTEM

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SLIDE 5

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT STATUS REPORT

FIELD COVERAGE AND VIGNETTING

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Cassegrain Focus Nasmyth Focus

φ~20 arcmin φ~14 arcmin

Science FoV: 14’ x 14’ Science FoV: 10’ x 10’

MOIRCS

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SLIDE 6

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT STATUS REPORT

ULTIMATE GLAO SYSTEM: EXPECTED PERFORMANCE

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研究の背景：補償光学の現状

可視光での補償光学は技術的に難しく、 世界的にも未開拓分野 4/12

100億年前の銀河の見え方のシミュレーション 大気揺らぎの影響を受けたすばる望遠鏡での観測 ハッブル宇宙望遠鏡 (赤外線) 現在のレーザー補償光学を用いたすばる望遠鏡での観測 すばる望遠鏡の可視光での回折限界

0.6秒角 0.2秒角 0.06秒角 0.02秒角

すばる望遠鏡の赤外線での回折限界

現状の限界 本研究で開拓

2018年打ち上げ予定のJWST宇宙望遠鏡でも 可視域の観測は感度が悪い

研究の背景：補償光学の現状

可視光での補償光学は技術的に難しく、 世界的にも未開拓分野 4/12

100億年前の銀河の見え方のシミュレーション 大気揺らぎの影響を受けたすばる望遠鏡での観測 ハッブル宇宙望遠鏡 (赤外線) 現在のレーザー補償光学を用いたすばる望遠鏡での観測 すばる望遠鏡の可視光での回折限界

0.6秒角 0.2秒角 0.06秒角 0.02秒角

すばる望遠鏡の赤外線での回折限界

現状の限界 本研究で開拓

2018年打ち上げ予定のJWST宇宙望遠鏡でも 可視域の観測は感度が悪い

Seeing (0”.5) GLAO (0”.2)

Probability of seeing and GLAO corrected FWHM

K-band

Improvement as a function of seeing factor of ~2 improvement at any seeing GLAO improvement uniformity Uniform over 14’x14’ FoV ULTIMATE GLAO performance has been proved by end to end numerical simulation. diffraction limited Hubble Space Telescope Median FWHM with GLAO ~ 0”.2 at K-band

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SLIDE 7

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT STATUS REPORT

NEW WIDE-FIELD NIR INSTRUMENTS PLAN FOR ULTIMATE

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MOIRCS

  • Reuse MOIRCS at Ns. IR

Phase 1

  • GLAO first light instrument
  • FoV ~ 4’ x 7’ (0”.12/pix)
  • Wavelength: 0.9 - 2.5 um
  • Imager/MOS spec (R500-3000)

2025

Multi-IFU concept by AAO

  • Fiber-bundle multi-IFU at Cs

Phase 3

  • Unique instrument for large

kinematic survey like MANGA/SAMI.

  • Feed to the existing spectrograph

(MOIRCS, R500-3000)

  • Patrol field: ~ 14’ x 14’
  • IFU FoV: 1”.2 x 1”.2
  • Number of IFUs: 8-13
  • Wavelength: 0.9 - 1.8 um

2030 2027

Imager concept by HIA

  • Wide-field imager (WFI) at Cs.

Phase 2

  • Workhorse instrument for large

imaging survey

  • FoV ~ 14’ x 14’ (~0”.1/pix)
  • Wavelength: 0.9-2.5 um
  • Wide-variety of narrow/medium

band filters

Conceptual design studies are ongoing

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SLIDE 8

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT OVERVIEW

WFI CONCEPTUAL DESIGN

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Conceptual optical design (Single barrel) Currently achieved image quality:Not optimized yet

  • WFI conceptual design (optical, opto-

mechanical,cryogenic) is on-going

  • Design started from a single barrel design
  • Not yet achieved the required image quality
  • Largely limited by the availability of large optics

(Fused Silica~600mm, CaF2~400mm)

  • Optional design to split the field into 4

Wavelength 0.95-2.5 micron Field Coverage 14’ x 14’ Image Quality FWHM<0”.1 Pixel Scale 0”.1/pix Throughput 0.5-0.6

Tentative Specification for WFI

CoDR in the middle of 2020

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SLIDE 9

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT STATUS REPORT

ULTIMATE SUBARU PROJECT TIMELINE

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ULTIMATE NB imaging

GLAO + MOIRCS (~FY2025) = ULTIMATE-Subaru Phase-I Wide Field Imager (~FY2027) = ULTIMATE-Subaru Phase-II Multi-IFU Instrument (~FY2029) = ULTIMATE-Subaru Phase-III Component 1 Component 2 Component 3

GIRMOS-like? Canadian MOS?

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SLIDE 10

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT OVERVIEW

OTHER CAPABILITY: NARROW FIELD, BUT WIDE WAVELENGTH RANGE

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Laser Tomography AO with ASM

Field Coverage: several arcsec Image Quality: FWHM<0”.1, SR~0.1@750nm

  • Good Image Quality throughout the range from

visible to NIR

  • Best for X-shooter like wide-wavelength range

spectrograph with “ULTIMATE” sensitivity ==> D-shooter (Daughter of X-shooter) D-shooter expected sensitivity

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SLIDE 11

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT STATUS REPORT

ULTIMATE-SUBARU: CURRENT ACTIVITIES

▸ ULTIMATE has been started: ▸ JSPS grant (Kiban-S: ~1.6M USD for 5 years) has been allocated for

ULTIMATE-START project ▸ Key subsystem demonstration: 4 Laser Guide Stars, 4 SH-WFS, laser tomography

▸ AO188 upgrade projects were funded internally at Subaru ▸ AO188 LGS upgrade with TOPTICA fiber laser

▸ Implement a GPU-based real-time system (CACAO) for AO188

▸ GLAO system Conceptual Design has been completed in FY2018

▸ Collaboration with Tohoku Univ, ANU, and ASIAA for GLAO CoDR studies ▸ GLAO Conceptual Design Review on Oct. 8 and 9, 2018

▸ Next step (FY2019-FY2021)

▸ GLAO preliminary design phase ▸ WFI conceptual and preliminary design phase ▸ WFS and semi-conductor laser prototyping and test

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NAOJ’s A-project approved for GLAO development part

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SLIDE 12

NIR survey WS (07/01/2019)

ULTIMATE-SUBARU PROJECT STATUS REPORT

A-PROJECT MISSION AND CHARGES

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SLIDE 13

ULTIMATE-SUBARU SCIENCE GOALS

ULTIMATE-SUBARU SCIENCE

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SLIDE 14

ULTIMATE-SUBARU SCIENCE

ULTIMATE-SUBARU SCIENCE TEAM (~70 SCIENTISTS)

Toshiki Saito (MPIA) Sarah Leslie (ANU) Chien-Hsiu Lee (Subaru/NOAO) Chris Lidman (AAO) Yen-Ting Lin (ASIAA) Yuichi Matsuda (NAOJ) Noriyuki Matsunaga (Tokyo) Yoshiki Matsuoka (Ehime) Yosuke Minowa (Subaru) Takashi Moriya (NAOJ) Kentaro Motohara (Tokyo) Tohru Nagao (Ehime) Kimihiko Nakajima (NAOJ) David Nataf (ANU) Chow-Choong Ngeow (NCU) Shogo Nishiyama (Miyagi Educ.) Yumiko Oasa (Saitama) Masamune Oguri (IPMU) Sakurako Okamoto (Subaru) Masato Onodera (Subaru) Tae-soo Pyo (Subaru) Christian E. Rusu (Subaru) Toshiki Saito (MPIA) Adam Schaefer (ANU) Takatoshi Shibuya (Kitami Inst. Tec.) Rhythm Shimakawa (Subaru) Kazuo Sorai (Hokkaido) Takahiro Sumi (Osaka) Daisuke Suzuki (JAXA) Tomoko Suzuki (Tohoku) Ken-ichi Tadaki (NAOJ) Tsutomu T. Takeuchi (Nagoya) Ichi Tanaka (Subaru) Masaomi Tanaka (NAOJ) Masayuki Tanaka (NAOJ) Tsuyoshi Terai (Subaru) Yoshiki Toba (ASIAA) Kazufumi Torii (NAOJ) Junko Ueda (NAOJ) Kenneth C. Wong (NAOJ) Takuji Yamashita (Ehime) Kiyoto Yabe (IPMU) Chikako Yasui (NAOJ) Tiantian Yuan (ANU) Tayyaba Zafar (Macquarie) Masayuki Akiyama (Tohoku) Fuyan Bian (ANU) Jessica Bloom (Sydney) Julia Bryant (AAO)

  • D. Calzetti (Massachusetts)

Andy Casey (ANU) Masashi Chiba (Tohoku) Scott Croom (Sydney) Akihiko Fukui (NAOJ) Olivier Guyon (Subaru) Akio Inoue (Waseda) Daisuke Iono (NAOJ) Masatoshi Imanishi (NAOJ) Ikuru Iwata (Subaru) Masao Hayashi (NAOJ) I-Ting Ho (ANU) AkIo Inoue (Waseda) Hiroyuki Kaneko (NAOJ) Lisa Kewley (ANU) Satoshi Kikuta (SOKENDAI) Ji-Hoon Kim (Subaru) Jin Koda (Stony Brook) Tadayuki Kodama (Tohoku) Kotaro Kohno (IoA, Tokyo) Naoki Koshimoto (Osaka) Yusei Koyama (Subaru)

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SLIDE 15

ULTIMATE-SUBARU SCIENCE

ULTIMATE-SUBARU = GLAO + NEW IR INSTRUMENT

NIR (K-band) facilities available in 2020s and beyond.

[typical classical AO] [w/ GRAAL]

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SLIDE 16

ULTIMATE-SUBARU SCIENCE

ULTIMATE-SUBARU IMAGING SENSITIVITY (TBD)

Note: still in conceptual design phase for WFI – remain uncertainty for instrument throughput.

~0.7-mag sensitivity improvement with improved image quality of GLAO

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SLIDE 17

ULTIMATE-SUBARU SCIENCE

UNIQUE CAPABILITIES OF ULTIMATE

MOIRCS

ULTIMATE

JWST

ULTIMATE has >20x survey power than JWST !

NB imaging K imaging

  • Narrow- & medium-band imaging (1.0<l<2.3um)
  • Broad-band imaging at K-band
  • High-resolution MOS spectroscopy at H+K (Phase-I w/ MOIRCS)
  • AO-assisted multi-object IFU at J + H (+ K) (Phase-3)
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SLIDE 18

ULTIMATE-SUBARU SCIENCE

KEY SCIENCE: “BIRTH”, “GROWTH”, “DEATH” OF GALAXIES IN THE CRADLE OF COSMIC STRUCTURE

  • 1. First galaxies (birth)

Ø Unprecedentedly deep imaging to detect galaxies at “cosmic dawn” (z>>7), as extension of LAE/LBG survey with HSC

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

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SLIDE 19

ULTIMATE-SUBARU SCIENCE

KEY SCIENCE: “BIRTH”, “GROWTH”, “DEATH” OF GALAXIES IN THE CRADLE OF COSMIC STRUCTURE

  • 1. First galaxies (birth)

Ø Unprecedentedly deep imaging to detect galaxies at “cosmic dawn” (z>>7), as extension of LAE/LBG survey with HSC

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

  • 2. Stellar build-up (growth)

Ø Deep & sharp & panoramic NB Ha/[OIII] imaging galaxies at “cosmic noon”(z=0.5-3.5)

Galaxies at z=4 WFIRST ULTIMATE GLAO seeing

SF galaxies @ z=2

Ø Tracking down the rest-optical SEDs of galaxies @ z~5 with BB/MB imaging (in K-band).

  • 3. Quenching (death)
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SLIDE 20

ULTIMATE-SUBARU SCIENCE

KEY SCIENCE: “BIRTH”, “GROWTH”, “DEATH” OF GALAXIES IN THE CRADLE OF COSMIC STRUCTURE

  • 1. First galaxies (birth)

Ø Unprecedentedly deep imaging to detect galaxies at “cosmic dawn” (z>>7), as extension of LAE/LBG survey with HSC

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

  • 2. Stellar build-up (growth)

Ø Deep & sharp & panoramic NB Ha/[OIII] imaging galaxies at “cosmic noon”(z=0.5-3.5)

Galaxies at z=4 WFIRST ULTIMATE GLAO seeing

SF galaxies @ z=2

Ø Tracking down the rest-optical SEDs of galaxies @ z~5 with BB/MB imaging (in K-band).

  • 3. Quenching (death)
  • 4. End products

Ø Complete census of ~60 nearby galaxies @ D<11Mpc with BB+NB.

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SLIDE 21

ULTIMATE-SUBARU SCIENCE

ULTIMATE FOR A VARIETY OF SCIENCE IN OUR GALAXY: GALACTIC CENTER & STAR-FORMING REGIONS

(C.H. Lee, D.Suzuki) (M. Chiba) (S. Nishiyama) (T. Pyo) (K. Torii) (C. Yasui) (Y. Oasa)

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SLIDE 22

ULTIMATE-SUBARU SCIENCE

TIME DOMAIN ASTRONOMY IN ULTIMATE ERA

(Moriya et al. 2019)

Supernovae search at z>6 – visiting 1-deg2 every 180-days down to K > 26 mag (AB) will allow us to detect PopIII pair-instability SNe at 6<z<7.

Note: the finally combined image from this survey will reach K~27.5 (AB mag)

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SLIDE 23

ULTIMATE-SUBARU SCIENCE

PRELIMINARY SURVEY DESIGN

  • 1. ULTIMATE Deep Legacy

Survey (UDLS) covering ~2- deg^2 overlapped with HSC U-Deep and PFS deep survey area with FWHM<0.25”.

  • 2. ULTIMATE nearby galaxy

atlas survey for 60 galaxies with various physical parameters with FWHM<0.5-arcsec.

seeing

(assuming the framework of Subaru SSP)

NB(JHK) MB (K) BB (K) NB BB

GLAO

“PREMIUMS”: Panoramic REsearch with Multi-band Imaging by ULTIMATE Machine on Subaru

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SLIDE 24

ULTIMATE-SUBARU SCIENCE

SUMMARY

▸ ULTIMATE-Subaru = Development of GLAO + new NIR instrument

▸ FWHM=0.2” over ~20-arcmin @ K-band in median conditions ▸ NAOJ A-project from FY2019

▸ Uniqueness of ULTIMATE-Subaru:

▸ NB & MB imaging (1.0<l<2.3um) ▸ Broad-band K-band imaging ▸ High-resolution MOS / multi-object IFU spectroscopy (phase 1 and 3)

▸ Key science goals – “birth”, “growth”, “death” of galaxies:

▸ [1] Birth : galaxies at z>>7 with NB Lya imaging ▸ [2] Growth : NB Ha mapping within galaxies in the cosmic noon ▸ [3] Death : massive/passive galaxies out to z~5 with MB imaging ▸ [4] End products: complete census of nearby galaxies (D<20Mpc)

▸ A variety of science goals achievable with ULTIMATE:

▸ Our Galaxy – particularly Galactic Center and star-forming regions ▸ Time domain science with NIR in 2020s-2030s ▸ Very sensitive single-object spectroscopy (simultaneously optical-NIR) with LTAO mode