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

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) プロジェクトの概要 ULTIMATE-Subaru \

ULTIMATE-SUBARU PROJECT OVERVIEW SUBARU STRATEGIC PLAN TOWARD 2020 AND BEYOND Recommendation from Subaru Science Advisory Committee 1. Very wide-field optical imager HSC (2013) 2. Wide-field multi-objet spectrograph PFS (~2021) 3. Wide-field NIR imager and MOS/IFU spectrograph w/ AO ULTIMATE(~2026) Dark nights Bright nights PFS Spec. (~2021-) ULTIMATE (~2026-) HSC Img. (2013-) 2 1 λ [um] ULTIMATE = U LTRA-WIDE-FIELD L ASER T OMOGRAPHIC I MAGER and M OS with A O for T RANSCENDENT E XPLORATION by SUBARU NIR survey WS (07/01/2019) � 2

https://www.eso.org/sci/facilities/develop/ao/ao_modes/.html ULTIMATE-SUBARU PROJECT STATUS REPORT WIDE-FIELD ADAPTIVE OPTICS: GLAO ���� ������ Turbulence profile at MaunaKea NIR survey WS (07/01/2019) � 3

ULTIMATE-SUBARU PROJECT STATUS REPORT ULTIMATE-SUBARU GLAO SYSTEM NIR survey WS (07/01/2019) � 4

Cassegrain Focus Nasmyth Focus φ~20 arcmin φ~14 arcmin Science FoV: 14’ x 14’ Science FoV: 10’ x 10’ MOIRCS ULTIMATE-SUBARU PROJECT STATUS REPORT FIELD COVERAGE AND VIGNETTING NIR survey WS (07/01/2019) � 5

100億年前の銀河の見え方のシミュレーション 0.2秒角 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 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 0.06秒角 可視域の観測は感度が悪い 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) 研究の背景：補償光学の現状 4/12 2018年打ち上げ予定のJWST宇宙望遠鏡でも 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 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 本研究で開拓 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) 100億年前の銀河の見え方のシミュレーション すばる望遠鏡の可視光での回折限界 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 0.6秒角 ULTIMATE-SUBARU PROJECT STATUS REPORT ULTIMATE GLAO SYSTEM: EXPECTED PERFORMANCE ULTIMATE GLAO performance has been proved by end to end numerical simulation. Hubble Space Telescope diffraction limited Improvement as a function of seeing factor of ~2 improvement at any seeing K-band Probability of seeing and GLAO corrected FWHM GLAO improvement uniformity Uniform over 14’x14’ FoV Median FWHM with GLAO ~ 0”.2 at K-band NIR survey WS (07/01/2019) � 6

• Feed to the existing spectrograph • Wide-variety of narrow/medium • FoV ~ 14’ x 14’ (~0”.1/pix) imaging survey • Workhorse instrument for large Phase 2 • Wide-field imager (WFI) at Cs. Imager concept by HIA 2027 2030 • Wavelength: 0.9 - 1.8 um • Number of IFUs: 8-13 • IFU FoV: 1”.2 x 1”.2 • Patrol field: ~ 14’ x 14’ (MOIRCS, R500-3000) kinematic survey like MANGA/SAMI. • Unique instrument for large Phase 3 • Fiber-bundle multi-IFU at Cs Multi-IFU concept by AAO 2025 • Imager/MOS spec (R500-3000) • Wavelength: 0.9 - 2.5 um • FoV ~ 4’ x 7’ (0”.12/pix) • GLAO first light instrument Phase 1 • Reuse MOIRCS at Ns. IR MOIRCS band filters • Wavelength: 0.9-2.5 um ULTIMATE-SUBARU PROJECT STATUS REPORT NEW WIDE-FIELD NIR INSTRUMENTS PLAN FOR ULTIMATE Conceptual design studies are ongoing NIR survey WS (07/01/2019) � 7

ULTIMATE-SUBARU PROJECT OVERVIEW WFI CONCEPTUAL DESIGN Conceptual optical design (Single barrel) Tentative Specification for WFI 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 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 CoDR in the middle of 2020 NIR survey WS (07/01/2019) � 8

GLAO + MOIRCS (~FY2025) Wide Field Imager (~FY2027) = ULTIMATE-Subaru Phase-I = ULTIMATE-Subaru Phase-II Multi-IFU Instrument (~FY2029) = ULTIMATE-Subaru Phase-III ULTIMATE-SUBARU PROJECT STATUS REPORT ULTIMATE SUBARU PROJECT TIMELINE Component 3 Component 1 Component 2 GIRMOS-like? Canadian MOS? ULTIMATE NB imaging NIR survey WS (07/01/2019) � 9

ULTIMATE-SUBARU PROJECT OVERVIEW OTHER CAPABILITY: NARROW FIELD, BUT WIDE WAVELENGTH RANGE Laser Tomography AO with ASM • 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 Field Coverage: several arcsec Image Quality: FWHM<0”.1, SR~0.1@750nm NIR survey WS (07/01/2019) � 10

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) NAOJ’s A-project ▸ GLAO preliminary design phase approved for GLAO ▸ WFI conceptual and preliminary design phase development part ▸ WFS and semi-conductor laser prototyping and test NIR survey WS (07/01/2019) � 11

ULTIMATE-SUBARU PROJECT STATUS REPORT A-PROJECT MISSION AND CHARGES NIR survey WS (07/01/2019) � 12

ULTIMATE-SUBARU SCIENCE ULTIMATE-SUBARU SCIENCE GOALS

ULTIMATE-SUBARU SCIENCE ULTIMATE-SUBARU SCIENCE TEAM (~70 SCIENTISTS) Masayuki Akiyama (Tohoku) Toshiki Saito (MPIA) Adam Schaefer (ANU) Fuyan Bian (ANU) Sarah Leslie (ANU) Takatoshi Shibuya (Kitami Inst. Tec.) Jessica Bloom (Sydney) Chien-Hsiu Lee (Subaru/NOAO) Rhythm Shimakawa (Subaru) Julia Bryant (AAO) Chris Lidman (AAO) Kazuo Sorai (Hokkaido) D. Calzetti (Massachusetts) Yen-Ting Lin (ASIAA) Takahiro Sumi (Osaka) Andy Casey (ANU) Yuichi Matsuda (NAOJ) Daisuke Suzuki (JAXA) Masashi Chiba (Tohoku) Noriyuki Matsunaga (Tokyo) Scott Croom (Sydney) Tomoko Suzuki (Tohoku) Akihiko Fukui (NAOJ) Yoshiki Matsuoka (Ehime) Ken-ichi Tadaki (NAOJ) Olivier Guyon (Subaru) Yosuke Minowa (Subaru) Tsutomu T. Takeuchi (Nagoya) Akio Inoue (Waseda) Takashi Moriya (NAOJ) Ichi Tanaka (Subaru) Daisuke Iono (NAOJ) Kentaro Motohara (Tokyo) Masaomi Tanaka (NAOJ) Masatoshi Imanishi (NAOJ) Tohru Nagao (Ehime) Masayuki Tanaka (NAOJ) Ikuru Iwata (Subaru) Kimihiko Nakajima (NAOJ) Tsuyoshi Terai (Subaru) Masao Hayashi (NAOJ) David Nataf (ANU) Yoshiki Toba (ASIAA) I-Ting Ho (ANU) Chow-Choong Ngeow (NCU) Kazufumi Torii (NAOJ) AkIo Inoue (Waseda) Hiroyuki Kaneko (NAOJ) Shogo Nishiyama (Miyagi Educ.) Junko Ueda (NAOJ) Lisa Kewley (ANU) Yumiko Oasa (Saitama) Kenneth C. Wong (NAOJ) Satoshi Kikuta (SOKENDAI) Masamune Oguri (IPMU) Takuji Yamashita (Ehime) Ji-Hoon Kim (Subaru) Sakurako Okamoto (Subaru) Kiyoto Yabe (IPMU) Jin Koda (Stony Brook) Masato Onodera (Subaru) Chikako Yasui (NAOJ) Tadayuki Kodama (Tohoku) Tae-soo Pyo (Subaru) Tiantian Yuan (ANU) Kotaro Kohno (IoA, Tokyo) Christian E. Rusu (Subaru) Tayyaba Zafar (Macquarie) Naoki Koshimoto (Osaka) Toshiki Saito (MPIA) Yusei Koyama (Subaru)

ULTIMATE-SUBARU SCIENCE ULTIMATE-SUBARU = GLAO + NEW IR INSTRUMENT NIR (K-band) facilities available in 2020s and beyond. [typical classical AO] [w/ GRAAL]

ULTIMATE-SUBARU SCIENCE ULTIMATE-SUBARU IMAGING SENSITIVITY (TBD) ~0.7-mag sensitivity improvement with improved image quality of GLAO Note: still in conceptual design phase for WFI – remain uncertainty for instrument throughput.

ULTIMATE-SUBARU SCIENCE UNIQUE CAPABILITIES OF ULTIMATE 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) ULTIMATE has >20x survey power than JWST ! MOIRCS ULTIMATE JWST NB imaging K imaging