ULTIMATE-Subaru: Project Status Report · 2019-02-06 · ULTIMATE-SUBARU PROJECT OVERVIEW ULTIMATE-SUBARU: CURRENT ACTIVITIES ULTIMATE has been kicked off JSPS grant (Kiban-S: ~1.6M

Yosuke Minowa (Subaru Telescope)

ULTIMATE-Subaru working groupon behalf of

Michitoshi Yoshida (Director, Subaru) Yusei Koyama, Ikuru Iwata, Yoshito Ono, Takashi Hattori, Christophe Clergeon, Etsuko Mieda, Hirofumi Okita Ichi Tanaka, Naruhisa Takato, Nobuo Arimoto (Subaru),

Yutaka Hayano, Shin Oya, Hideki Takami (NAOJ), Masayuki Akiyama, Tadayuki Kodama,(Tohoku)

Kentaro Motohara (Univ. of Tokyo) Francois Rigaut, Celine D’orgeville, Gaston

Gausachs, Nick Herrald, Visa Korkiakoski (ANU) Shiang-Yu Wang, Chi-Yi Chou (ASIAA)

GLAO Conceptual Design Review @ Subaru Oct. 8-10, 2018

ULTIMATE-Subaru: Project Status Report

\

Subaru User’s meeting FY2018 (01/29/2019)

ULTIMATE-SUBARU PROJECT STATUS

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ULTIMATE-SUBARU: “WIDE-FIELD + HIGH-RESOLUTION” NIR INSTRUMENT WITH GLAO

Subaru/MOIRCS(4’x7’)

VLT/HAWK-I(7.5’x7.5’)

Subaru/IRCS(1’x1’)

HST/WFC3(2.0’x2.3’)

JWST/NIRCAM(2x2.2’x2.2’)

ULTIMATE-Subaru(14’x14’)

~100 Mpc scale

Seeing GLAO(0”.2)

SF galaxies@z~2~1kpc scale

Subaru will become survey telescope to provide “legacy data”

using HSC, PFS (in dark nights), and ULTIMATE (in bright nights)



WIDE-FIELD ADAPTIVE OPTICS: GLAO

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

��

Turbulence profile at MaunaKea


ULTIMATE-SUBARU PROJECT OVERVIEW

DIRECTION OF AO DEVELOPMENT AT THE EXISTING 8M TELESCOPES

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FoV （arcsec2)

Strehl Ratio

10 103 105102 104

High-contrast

Diffraction limited

Seeing improvement

MCAO MOAOLTAO

GLAO

ExAO

Classical AO systems

SCExAO(Subaru)GPI(Gemini-S) SPHERE(VLT) KPIC(Keck)

GALACSI (VLT) KAPA (KECK)ULTIMATE-START (Subaru)

GEMS (GEMINI-S) MAVIS (VLT) ??? (GEMINI-N)

GIRMOS (GEMINI-S)

GRAAL/GALACSI (VLT) ULTIMATE (Subaru)



GLAO BASELINE SPECIFICATIONS

▸ Use conventional SH-WFS as baselines for both LGS and NGS WFS▸ Well-developed Adaptive Secondary Mirror is used. ▸ Low technical challenge in sub-system level development ▸ Main challenge is coming from the wide-field coverage

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CONCEPTUAL DESIGN REVIEWULT.CDR.AO.DOC.3.GLAOVersion 1.0.0

ULTIMATE

Figure 11: Network configuration of the Subaru telescope.

unit of the TOPTICA laser has been already delivered to Subaru to upgrade the existing LGSFfor the facility AO system (see Section A.2). The second TOPTICA laser will be procured by thetime of the ULTIMATE GLAO assembly and integration. Alternatively, we are considering to usea semiconductor laser being developed by Australian National University (ANU) as a second lasersystem (see Section 7.3 for more details). The LGS and NGS wavefront sensor systems will beinstalled at both Nasmyth and Cassegrain to feed the GLAO corrected image at both focus (seeSection 7.2 for more details). Baseline specification of the ULTIMATE-Subaru GLAO system issummarized in Table 2.

3.3 Science instrument plan

The instrument suites that we are currently considering for the ULTIMATE-Subaru are wide-fieldimager, multi-object slit spectrograph, and multi-object integral field unit (IFU) spectrograph,

Table 2: GLAO baseline specificationItem SpecificationGuide Star 4 LGSs (⇠ 10 W for each, ⇠ 500 photons/cm2/sec)

4 NGSs (r < 19mag)Technical FoV LGS: edge of FoV (r < 100 at Cs, r < 70 at Ns)

NGS: 4 crescent areas at the outside of science FoVWFS LGS: 32⇥32 Shack-Hartmann (0.006/pix)

NGS: 2⇥2 Shack-Hartmann (Visible, 0.0015/pix)WFS frame rate > 500 HzDeformable mirror Adaptive Secondary with ⇠ 1000 actuators

Page 22 of 166



FIELD COVERAGE AND VIGNETTING

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Cassegrain Focus Nasmyth Focus

φ~20 arcmin φ~14 arcminScience FoV: 14’ x 14’ Science FoV: 10’ x 10’

MOIRCS



ULTIMATE GLAO: KEY SUB-SYSTEMS

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TOPICA fiber laser (589nm) x 2 Generate 4 LGS asterism Laser Guide Stars

Cass. Focus (FoV~20 arcmin ∅)

Wavefront sensors

Nasmyth IR Focus (FoV~14 arcmin ∅)

YM’s poster for conceptual design of the subsystems

Adaptive Secondary Mirror

Preliminary Subaru ASM with 924 actuators design by Adoptica



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)

Y. Ono’s poster for more details about the performance simulation

Probability of seeing and GLAO corrected FWHM

K-band

Improvement as a function of seeingfactor of ~2 improvement at any seeing

GLAO improvement uniformityUniform over 14’x14’ FoV

ULTIMATE GLAO performance has been proved by end to end numerical simulation.



NEW WIDE-FIELD NIR INSTRUMENTS PLAN FOR ULTIMATE

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MOIRCS

• Reuse MOIRCS at Ns. IRPhase 1

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

2025

130

Table 7.7: Instrument parameters of Starbug based IFU spectrographIFUs

Number of IFUs 8-13a

Number of elements per IFU 61 Hexagonally packedSpatial sampling per element 0.15 arcsecTotal field of view per IFU 1.18 square arcsecTotal patrol area φ ∼ 15 arcminb

Minimum separation between IFUs 25 arcsecSpectrograph (MOIRCS)

Wavelength coverage 0.9-1.8 µmSpectral resolving power 500-3000Dispersion 1.6 A per pix (J), 2.1 A per pix (H)Sampling 2-5 pixels in FWHM

Combined propertiesTotal efficiency 9% (J), 12% (H)a This number can be increased by using a new larger spectrograph.b FoV of the wide field corrector.

Figure 7.16: Block diagram of the starbug-based multi fiber IFU system, showing the sub-systems.

130

Multi-IFU concept by AAO

• Fiber-bundle multi-IFU at CsPhase 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

20302027

116

7.2

Wid

e-field

Imager

Takash

iH

attori 1,Joh

nPazd

er2,

Tom

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uro

3,an

dY

okoTan

aka1

1Subaru

Telescope,NationalA

stronomicalO

bservatoryofJapan,

2H

erzbergInstitute

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ationalResearch

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anada,3

OptC

raft

7.2

.1Four

barrel

imager

desig

n(J

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Here

we

summ

arizea

conceptualstudy

byJohn

Pazder

(NR

C-N

SI-AST

/HIA

)based

onhis

technicalnote

”Subaruconcentric

correctorand

fourbarrelG

LAO

imager

OpticalD

esignC

oncept”(5/29/2013).

Because

theavailable

field-of-viewat

SubaruC

assegrainfocus

was

stillunder

studyat

thetim

ew

henthis

technicalnotew

asw

ritten,∼φ20

′isassum

edin

thisstudy.

The

concentriccorrector

consistsof

two

elements

ofInfrasil-302

with

sphericalsurfaces

and690m

min

diameter.

Itprovides

auniversal

22′.8

diameter

fieldof

view(at

f/12.4)w

ithresidual

opticaldesign

aberrationsless

than66m

as.T

hiscorrector

isdesigned

tofeed

multi-barrelopticalsystem

sw

ithoutpupil

miss-m

atch.T

heim

agerdesign

conceptis

afour-barrel

imaging

systemfeed

bythis

correctorw

itheach

barrelhaving

a4k×

4kH

4RG

detectorcovering

a6′.8

×6′.8

fieldof

view(0

′′.1/pixelsam

pling).T

hetotal

imager

fieldofview

is185

squarearc

minutes.

Figure

7.1show

sthe

opticallayoutofthis

system.

The

cameras

arew

ithina

volume

of2.1m

inlength

and0.8

min

diameter.

Aw

indowhas

beenput

atthe

entranceto

thecam

eras,with

theintention

ofthecam

erasbeing

enclosedin

theD

ewar

with

thecorrector

andw

avefront

sensorsoutside

theD

ewar.

The

cameras

havebeen

designedw

itha

sharppupilim

age.

Figure

7.1:O

pticallayoutofthe

correctorand

imager

system(J.P

azder,section7.2.1)

The

image

qualityis

shown

inFigure

7.2.Spot

qualityis

lessthan

pixelsat

allpoints

exceptat

theoutside

cornerw

herethe

image

qualityis

marginally

more

at16

µmR

MS

spotdiam

eter.

116

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



ULTIMATE-SUBARU: CURRENT ACTIVITIES▸ ULTIMATE has been kicked off▸ JSPS grant (Kiban-S: ~1.6M USD for 5 years) has been allocated for

ULTIMATE-START project (Akiyama’s poster for more detail)▸ 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 (Mieda’s talk)▸ Implement a GPU-based real-time system (CACAO) for AO188 (Clergeon’s poster)

▸ 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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Applied for NAOJ’s A-project from FY2019



SUMMARY▸ Wide-field and High-resolution in NIR are essential to reveal the complete

history of galaxy evolution ▸ GLAO at Mauna Kea is the best to achieve this capabilities

▸ ULTIMATE-Subaru Project:▸ GLAO and wide-field NIR instruments, which provide ~14x14 arcmin2 FoV with ~0”.2

spatial resolution in K-band.▸ GLAO capabilities both at NsIR and Cs ▸ Key sub-systems: ASM, LGS, and 4 LGS and NGS SH-WFSs.

▸ Instrument development:▸ Develop GLAO at NsIR with the existing NIR instrument MOIRCS as a first step.

Expected first light: GLAO+MOIRCS in 2025.▸ GLAO at Cs and dedicated wide-field NIR instruments (WFI and M-IFS) will be developed

to provide the widest field coverage at later phases. GLAO+WFI in 2027▸ GLAO key components are being prototyped and demonstrated with AO188 upgrade

projects and ULTIMATE-START project (LTAO). ▸ Conceptual design has been done in collaboration with Tohoku, ANU, and ASIAA.

•

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Documents

ULTIMATE-Subaru: Project Status Report · 2019-02-06 · ULTIMATE-SUBARU PROJECT OVERVIEW ULTIMATE-SUBARU: CURRENT ACTIVITIES ULTIMATE has been kicked off JSPS grant (Kiban-S: ~1.6M