Tadayuki Kodama（on behalf of theULTIMATE-SUBARU team）

Ultra-wide-field Laser Tomographic Imager and MOS with AO forTranscendent Exploration by SUBARU telescope.

Future key instruments of Subaru Telescope
鼎（tripod pot）

PFS(opt)

HSC(opt)

ULTIMATE(NIR)ULTIMATE-SUBARU
1. Ground Layer AO with Adaptive
Secondary Mirror (4 LGSs)
2. Wide-field Near-IR Instrument(Imager, MOS or M-IFU)

4 laser guidestar
Adaptive
ScondaryMirror→ Seeing improvement(FWHM 0.4”→0.2”) over FOV ~15’
Higher sensitivity equivalent to 2x
telescope aperture*1
6 times wider FOV*2~200 times wider FOV comparedwith AO188/LGS+IRCS

1. Targeted to Start*1 For point sources.
Commissioning in 2020
*2 Relative to MOIRCS (seeing limited NIR instrument)

Wavefront
Sensor
NIR instrument3

0.2” (~1.5kpc) at K-band

Starbugs + IFU

Starbugs
Positioner+ Fibre bundles

ν
Wavelength range is limited to <2µm (no K-band)
Hα, [NII] limited to z<2, but [OIII], Hβ, [OII] to z~3Fibre Bundle Configuration
Number of fibres

61 (9 fibres on an axis)

Spatial sampling

0.2 arcsec / fibre

Bundle sky diameter

1.8 arcsec (point to point)

Number of detector pixels per fiber

4

Number of pixels per bundle

244

Number of bundles per 2k detector

8 (1952 pixels; plus sky fibers?)

Object Multiplicity (MOIRCS)

16

Sky fibres/detector

23 sky fibres plus 1 fibre gap

N=61 bundle (Bryant et al.
2014, MNRAS 438, 869)

A phased approach for ULTIMATE-SUBARU
Phase 0.5 = Starbugs (+WFC/metrology camera) w/o GLAO
+ NuMoirics (new detectors and new grating)+ Cassegrain modification (13’ x 8’)(decommission of FOCAS, ADC, AGSH?)
基盤Ｓ + NAOJ (Cass改造)

Phase 1 = phase 0.5 + GLAO (adaptive secondary)
新学術 + NAOJ ?

Phase 2 = New dedicated NIR imager and spectrograph withmore arrays and higher throughput + Wider CassFoV (15’x15’)
特別推進?

Phase 3 = Phase 2 + OH suppression fibres + K fibres

Science Brainstorming
Subaru next generation AO workshop(2011/9/8-9, Osaka Univ. Nakanoshima Center)
More general, including MOAO↓

Subaru GLAO Science Workshop 2012(2012/10/17-18, Subaru Hilo Office)
Kick-off meeting (invitation only)↓Subaru GLAO Science Workshop 2013(2013/6/13-14, Hokkaido University)
wider community including Canadians, key science, imager/MOS↓

ULTIMATE-Subaru Science Workshop 2014(2014/7/28-29, NAOJ Mitaka)wider community including Australians, starbug&IFU system

SINS Survey
z~2 UV selected galaxies; VLT/SINFONIIFU分光によって、形成途上銀河の内部運動や物理過程が詳細に分かる。

Foerster-Schreiber et al. (2009)

銀河内部の星形成マップや化学進化から、星形成の伝搬（中心バースト?inside-out?）やガスの流入（cold-stream?）を探る
2D map of line ratios(metallicity indicators)
such as[OIII]/Hβ and [NII]/Hα

VLT/SINFONICresci et al. (2010)see also
Jones et al (2010)
With Keck2/OSIRIS

Lower metallicity at the center  Dilution by (almost) metal-free cold streams?

クランプ銀河からのガスのアウトフロー（フィードバックの現場）
Hα輝線
プロファイルblue wing = outflow

Genzel et al. (2011)
クランプBで起こっている星形成バーストによるガスのアウトフロー（~500km/s）

Ohta’s slide

波及効果
望遠鏡性能の一般的改善（主焦点装置以外）
可視（FOCAS）でもシーイング改善
熱背景光の低減（補償光学系のミラー枚数減）
Extreme-AO の開発
Laser-Tomography AOの開発
TMT時代に、日本の補償光学技術の維持、発展Summary & Discussion• Utilization of Subaru bright nights and reuse ofexisting instruments (e.g. MOIRCS)• Killer science in the era of TMT?
-Galaxy anatomy at 0<z<3 (in e.g. CANDELS/3DHST)-Lyα blobs/haloes (detection/size/kinematics)-Clusters/Proto-clusters• No K-band (<2µm)?
-Hα, [NII] limited to z<2, but [OIII], Hβ, [OII] to z~3• IFU or MOS? (K-band availability & multiplicity)-complex structure of high-z galaxies  IFU?
-slit scan with MOS? (slit loss, seeing variation…)• Decommission of ADC, AGSH, FOCAS ?

The END
See http://www.naoj.org/Projects/newdev/ngao/glaows14/

Backup slides

Wavelength range is limited to <2µm (no K-band)

1 µm

2 µm

Hα, [NII] limited to z<2, but [OIII], Hβ, [OII] to z~3

Metallicity gradient of red SF galaxies
Constant [NII]/Hα over the galaxies, but some hints of positive gradient?
CL0939-GMOS1

CL0939-GMOS2

CL0939-GMOS31” (5 kpc)

Koyama’s slide

CL0939-GMOS4

CL0939-GMOS5

Phase-0.5: Starbug+ New-MOIRCS w/o GLAO
Phase-1 :w/ GLAO
• Number of bundles:(1) HK500, zJ500, R1300+BB(JHK), VPH: 16(2) R1300 or VPH + Narrow-band or Intermediate band filters: 48

Sensitivity: 60-70% of MOSFIRE/Keck (MOIRCS VPH only)
Sensitivity: 75- 85% of KMOS/VLT (MOIRCS VPH only)
Need to multiply by 70-80% efficency for fibre system
MOIRCS will be moved to the observation floor or Nasmyth platform andconnected to the starbugs with fibres.
• Focal plane unit of MOIRCS will be modified to feed the light into slits from fibres.
••••Tadaki’s slideIs ULTIMATE-S really ULTIMATE?
• Do we really want ULTIMATE-Subaru while TMT
is coming along?
- TMT-AGE/IRMOS will beat us?
- What is the future of Subaru-IR?
- Excellent synergy with ALMA/JVLA(resolution, SFR depth…)?
- Expansion of Keck/Gemini/VLT timeexchange programmes?

Cost estimation, budget
Items

Cost

BudgetASM system

6M

Grant-in-aid Scientific Research, etc.

Laser system

0.5 – 4 M

Grant-in-aid Scientific Research, etc.
(if Rayleight LGSs, cost is 1/10)

Wavefront sensor unit

1M

Grant-in-aid Scientific Research(International collaboration)

Realtime controller

0.5 M

Grant-in-aid Scientific Research, etc.
(International collaboration)

Telescope modification

5–8M

NAOJ budget

NIR instrument0 – 10 M

Existing instrument at first.
(MOIRCS or MOIRCS upgrade etc.)

Manpower

2M

NAOJ budget and Grant-in-aid Scientific ResearchContingency

5M

Total

20 – 36.5 M

1. Grant-in-Aid for Scientific Research on Innovative Areas, 2015-2019
2. Grant-in-Aid for Specially Promoted Research, 2016-2020
3. Grant-in-Aid for Scientific Research (Category S), 2020-2024

Schedule
2012

1315

14161817

192020

Review
Review
Concept Design
Prelim Design

Review
Detail Design
FabricationFL

Telescope Modification
Integration and Test

Science Operation

AO188/LGSHSCPFS
TMTGLAO

Guide stars

Ground-Layer Adaptive Optics

Atmosphericturbulence
Turbulence atground layer
Feedback correction
to deformablesecondary mirror

Wavefrontsensors

Estimation ofground-layer
turbulence30Resolving power and FoV of our facilities
Subaru+AO188
0.06-0.1”@2μm (~0.5-1kpc @z>1), 1 arcmin (FoV)
Subaru+GLAO
0.2” @2μm (~1.5kpc),

15 arcmin

JWST0.05” @2μm (~0.5kpc),

3 arcmin

TMT+AO
0.015” @2μm (~0.1kpc),

15 arcsec

ALMA0.01-0.1”@Submm (0.1-1kpc),(0.08-0.6” in cycle-1)

10arcsec-1arcmin

Phase-I: Starbug+ New MOIRCS•First light instrument for GLAO•

Number of bundles:••••

Sensitivity: 60-70% of MOSFIRE/Keck (MOIRCS VPH only)
Sensitivity: 75- 85% of KMOS/VLT (MOIRCS VPH only)
Need to multiply by 70-80% efficency for fiber system
MOIRCS will be moved to the observation floor or Nasmyth platform andconnected to the starbugs with fibers.
Focal plane unit of MOIRCS will be modified so as to feed the light into slits fromfibers.

•– Commissioning obs. will start from around 2017?
– Observations with OH suppression 2020?.
– (1) HK500, zJ500, R1300+BB(JHK), VPH: 26 (config 1); 52 (config 2); 16 (config 3)– (2) R1300 or VPH + Narrow-band or Intermediate band filters: 78 (config 1); 156 (config 2); 48(config 3)

Phase-II: Starbug +new dedicatedinstrument• First light will be several years after GLAO commissioning• Number of bundles:– 52 (config 1); 104 (config 2); 32 (config 3) for each spectrograph!
– Φ13’.5 FOV• Sensitivity: 70-80% of MOSFIRE/Keck– Sensitivity of the spectrograph should be same as or higher than
MOSFIRE.
– Only difference is throughput and emissivity due to the fibers.
– Not including telescope diameter difference• New instrument will be placed on the observation floor or Nasmythplatform and connected to the starbugs with fibers.

Sensitivity comparison with MOSFIRE
MOIRCS
Current
FOVNew

MOSFIRE

4’x7’

6’.1x6’.1Imaging throughput(atm+Telescope+Instrument)

0.23(J), 0.34(H),0.30(K)0.54(J),0.56(H),0.50(K)Spectral resolution

500, 1300, ~3000(VPH)*

3500

Grating diffraction efficiency

HK500, zJ500: 0.8(J), 0.78(H), 0.65(K)R1300: 0.2(J), 0.3(H), 0.5(K)
VPH: ~0.75(J), ~0.7(H) 0.80(K)0.60(J), 0.65(H),0.70(K)Spec. throughput(atm+Telescope+Instrument)

HK500, zJ500: 0.18(J), 0.26(H), 0.20(K)
R1300: 0.05(J), 0.10(H), 0.15(K)
VPH: ~0.15(J), ~0.20(H), ~0.26(K)0.325(J), 0.361(H), 0.350(K)Detector

HAWAII-2QE

HAWAII-2RG~80%(JHK)

Read-out noise

15e rms(16NDR)

5e rms (16NDR)HAWAII-2RG~80%(JHK)
5e rms (16NDR)* For 0.5” slit. Using a fiber with 0.2” spatial sampling, resolutions are 2.5 times

Sensitivity Improvement of MOIRCS• HAWAII2 => H2RG
– Readout noise: 15e- => 5e-• Grism replacement– System throughput: 15%(R1300) => 25%(R2000)• Sharp and stable image with GLAO
• Improvement of emission line sensitivity– Point source: >1.2 mag. (>3x)– Extended source: ~0.5 mag. (~1.6x)

Sensitivity comparison with MOSFIRE• Current MOIRCS sensitivity is 4~7 times lower than MOSFIRE(difference in the telescope diameter is not taken into account).
• If the new MOIRCS can successfully reduce the RO-noise down to5e-, the sensitivity difference is about 1.4(VPH)~2.3(R1300).
• This difference can not be reduced without changing the opticalcoating.
– MOSFIRE has 31 surfaces– Average throughput in each surface is about 0.992.
– Total throughput of the optical coating is about 0.78
– MOIRCS has 24 surfaces.
– Average throughput of the coating is 0.983.
– Total throughput of the coating is 0.64.

Phase 1 = GLAO feeding fibre/IFU’s on NuMorics
Phase 2 = GLAO feeing new J,H,(K?) spectrograph (pupose-designed for this andOH-suppression fibres)
Phase 3 = same as Phase 2, but with OH suppression fibres.
There are a wide range of extragalactic science drivers. The main Australian driveris a follow-up to the SAMI survey at redshift > 1.0
NAOJ wishes to propose to the Kakehni grant in order to fund phase 0.5. Thisfunding could be as much as $2M USD in addition to $200-300K in internalfunds. Internal deadline is late September or early October, external deadline isNovember. To that end NAOJ would like AAO to produce a rough order ofmagnitude (ROM) schedule and budget to be included in this proposal. Thisbudget will be broken out in terms of:• Wide-field-corrector (which can possible be part of the telescope infrastructure
and therefore eligible for internal funds)• Starbugs IFU’s (16)• Fibre cable• Vacuum system• Electronic control system• Metrology system, including camera etc..
• Software packages for a) acquisition,b) control of starbugs c) metrology d) firstorder data-reduction
We are actively working on this and should have a reasonably accurate budget
within 4-6 weeks.

• Vacuum system• Electronic control system• Metrology system, including camera etc..
• Software packages for a) acquisition,b) control of starbugs c) metrology d) firstorder data-reduction
We are actively working on this and should have a reasonably accurate budget
within 4-6 weeks.
In addition, NAOJ would like to explore with AAO the possibility of K-bandfibres. NAOJ has requested funds for a K-band fibre. AAO is happy to discuss
how and when we could test this at AAO.
NAOJ also has a CoDR planned for end of this calendar year or early next year
to present the status of the entire GLAO project. AAO would be happy to help
prepare some materials on the fibre positioning system, IFU’s. OH-suppression
technology etc.. For this review.
There is the possibility that AAO can provide some internal labour funds for theproject in the likely event that Phase 0.5 is more expensive than the funding
available through Kakehni Grant. In that case it appears that while there is
probably no guaranteed time for this project, there is precedent for collaborator
time on the telescope on joint NAOJ/AAO projects. This should be spelled out inour MOU. In the meantime AAO is working on a science document describing
our science project (SAMI at z>1) in detail, and querying the likely Australian
Astronomers who would be part of this consortium.
AAO is excited and interested to work with NAOJ, as we have in the past withFMOS Echidna. This meeting has been an excellent first step in that process.

Program
Jul 28 (Mon)
13:00-13:40 Y. Hayano: Project Overview
13:40-14:00 S. Oya: GLAO performance simulation
14:00-14:30 Y. Minowa: Instrument specifications and sensitivities
14:30-15:15 A. Sheinis (AAO): IFUs with Starbug & fibre systemBreak
15:30-16:00 Science-1: C. Lidman (AAO)
16:00-16:30 Science-2: M. Akiyama (Tohoku)
16:30-17:00 Science-3: K. Ohta (Kyoto)
17:00-17:30 Discussion
19:00- Banquet at Kichijoji (Shirubei), Odakyu bus #91 at 18:16 (or 18:04) at NAOJ
Jul 29 (Tue)
09:30-10:00 Science-4: K. Motohara (Tokyo)
10:00-10:30 Science-5: T. Shibuya (Tokyo)
10:30-11:00 Science-6: Y. Koyama (JAXA)
Break
11:30-12:00 Science-7: K. Tadaki (NAOJ)
12:00-12:30 Science-8: K. Kohno (Tokyo)
Lunch
14:00-14:30 Science-9: Y. Matsuda (NAOJ)
14:30-15:00 Science-10: D. Iono (NAOJ)
15:00-16:00 Discussion