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ULTIMATE-SUBARU:( plngoa ilCUerhbEIT u, 9,e h bnstg
3/2 0 2- 1A 4 AMSgULTIMATE-SUBARU PROLOGUESUBARU STRATEGIC PLAN TOWARD 2030

Subaru is going to be a “wide-field survey oriented” telescope:

1. Very wide-field optical imager
2. Wide-field multi-object spectrograph
3. Wide-field NIR imager and MOS/IFU spectrograph w/ AO

Dark nights ()
Spec.

Img.

HSC (2013-)
PFS (2022-)
ULTIMATE (2026-)

Bright nights ()PFS (~2022-)

ULTIMATE(~2026-)

HSC (2013-)
1 λ [um]

2

ULTIMATE = ULTRA-WIDE-FIELD LASER TOMOGRAPHIC IMAGER and MOS with AO
for TRANSCENDENT EXPLORATION by SUBARUULTIMATE-SUBARU CONCEPTGLAO : WIDE-FIELD ADAPTIVE OPTICS ON SUBARU

Improve image quality over ~20-arcmin at everywhere on sky
FWHM~0.2” @ K-band = resolution of HST/WFIRST @ Y,J,H
GLAO(0.2”)

seeingK-band, Maunakea(c.f. 0.3”-0.4” @ VLT)

r~19-magNstar=1 2 3 4https://www.eso.org/sci/facilities/develop/ao/ao_modes/.html

(COSMOS)ULTIMATE-SUBARU CONCEPTULTIMATE-SUBARU KEY SUBSYSTEMS
2019年度より国立天文台Aプロとして発足「すばるGLAOプロジェクト」

2017-2021年度 科研費基盤(S)“ULTIMATE-START”
代表: 秋山正幸 [東北大]ULTIMATE-SUBARU UNIQUENESSULTIMATE-SUBARU = GLAO + NEW IR INSTRUMENT
NIR (K-band) facilities available in 2020s and beyond.

[typical classical AO][w/ GRAAL]ULTIMATE-SUBARU UNIQUENESSUNIQUE CAPABILITIES OF ULTIMATE-SUBARU••••

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 !

MOIRCSJWSTNB imaging

ULTIMATE

K imagingULTIMATE-SUBARU UNIQUENESSUNIQUE CAPABILITIES OF ULTIMATE-SUBARU••••

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 !

MOIRCSJWSTNB imaging

ULTIMATE

K imagingULTIMATE-SUBARU SCIENCEULTIMATE-SUBARU SCIENCE TEAM (>70 SCIENTISTS)
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)
Daisuke Iono (NAOJ)
Masatoshi Imanishi (NAOJ)
Ikuru Iwata (Subaru)
Yuichi Harikane (NAOJ)
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)

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)
Kazuyuki Ogura (Bunkyo)
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 (Tohoku)
Masayuki Tanaka (NAOJ)
Tsuyoshi Terai (Subaru)
Yoshiki Toba (Kyoto)
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)

ULTIMATE-SUBARU SCIENCEKEY SCIENCE: “BIRTH”, “GROWTH”, “DEATH” OFGALAXIES IN THE CRADLE OF COSMIC STRUCTURE
1. First galaxies (birth)Ø Explore the LAE/LBG world toward thefrontier redshifts (z>>7) with ultradeep NB/BB imaging in NIR)((-z=8.7 z=11.8
z=7.7 z=10.0

ULTIMATE-SUBARU SCIENCEKEY SCIENCE: “BIRTH”, “GROWTH”, “DEATH” OFGALAXIES IN THE CRADLE OF COSMIC STRUCTURE
1. First galaxies (birth)Ø Explore the LAE/LBG world toward thefrontier redshifts (z>>7) with ultradeep NB/BB imaging in NIR

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

Ø)((SF galaxies @ z=2-seeing

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

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

GLAOULTIMATEWFIRSTGalaxies at z=4

ULTIMATE-SUBARU SCIENCEKEY SCIENCE: “BIRTH”, “GROWTH”, “DEATH” OFGALAXIES IN THE CRADLE OF COSMIC STRUCTURE
1. First galaxies (birth)Ø Explore the LAE/LBG world toward thefrontier redshifts (z>>7) with ultradeep NB/BB imaging in NIR

z=8.7 z=11.8
z=7.7 z=10.0)((seeing

2. Stellar build-up (growth)
3. Quenching (death)Ø Tracking down the rest-optical SEDs of galaxies@ z~5 with BB/MB imaging (in K-band).

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

SF galaxies @ z=2-

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

4. End products

GLAO

ULTIMATEWFIRST
Galaxies at z=4

ULTIMATE-SUBARU SCIENCE

TIME DOMAIN ASTRONOMY IN ULTIMATE ERASupernovae 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.

(Moriya et al. 2019)
Note: the finally combined image from this survey will reach K>27.5 (AB mag) .

ULTIMATE-SUBARU SCIENCEPRELIMINARY SURVEY DESIGNULTIMATE-Deep~2-deg2, ~0.25”
NB/MB/BB(K) ~26 mag

ULTIMATE-UltraDeep~0.5-deg2, <0.2”
BB(K)>27 mag“PREMIUMS”
PanoramicREsearch withMulti-band
Imaging byULTIMATE
Machine on
SubaruPlease give us yourinputs to maximize
the legacy value of
ULTIMATE-Subaru,and to provide ourbest sample for TMT.

http://candels-collaboration.blogspot.com/2012/07/cosmos-cosmic-evolution-survey.html © NASA/ESA/Z. Levay

ULTIMATE-SUBARU SCIENCEULTIMATE FOR A VARIETY OF SCIENCE IN OUR GALAXY:GALACTIC CENTER & STAR-FORMING REGIONS(S. Nishiyama)(M. Chiba)(T. Pyo)(K. Torii)(C.H. Lee,D.Suzuki)(Y. Oasa)(C. Yasui)ULTIMATE-SUBARU SCIENCEULTIMATE IS NOT ONLY FOR WIDE-FIELD AO▸ Please also recognize our“narrow-mode” capability.
▸ Our LTAO mode can deliver
ultimately high spatial
resolution and high sensitivity
to your favorite target!

Narrow
Small field
field+ extreme
correction

Wide field+ moderatecorrection

Strehl ratio

FWHM

LTAO
GLAO
(0.2” @ K)
LTAO
(0.05” @ all l) 


GLAO

ULTIMATE-SUBARU SCIENCEULTIMATE IS NOT ONLY FOR WIDE-FIELD AO▸ Please also recognize ourNarrow
Small field
field+ extreme
correction

Wide field+ moderatecorrection“narrow-mode” capability.
▸ Our LTAO mode can deliver
Conceptof “D-SHOOTER”
for ULTIMATE
ultimatelyhighspatial (R~5,000)
resolution
andhigh sensitivity
to your favorite target!

MOSFIRE on Keck

Strehl ratio

FWHM

D-SHOOTER on ULTIMATE
LTAO

GLAO
(0.2” @ K)

T. Moriya, M. Ouchi, M. Tanaka, N. Tominaga, M. Yoshida, Y. Minowa,
Y. Koyama, N. Takato, K. Motohara, S. Ozaki, M. Akiyama, Y. Ono

LTAO(0.05” @ all l) 

GLAOULTIMATE SUMMARY

SUMMARYULTIMATE-Subaru2030    = HSC/PFS () + ULTIMATE ()

(GLAO)



(LTAO)• FWHM=0.2” @ K-band• FWHM=0.05” @ all opt-NIR• 20-arcmin FoV (diameter)• A few to ~10-arcsec FoV

••
/M

LTK
EAU
CU
FU H
UP/SUCUHUCUITTH