k-gmt prerunner instruments – m-y chun – sdss-ksg 2008 feb. 19 1 k-giant prerunner instruments...

K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19 1

K-Giant Prerunner Instruments

2008. Feb. 19.SDSS-KSG 워크샵

천무영


Giant Magellan TelescopeProject

GMT Institutions

• Carnegie Observatories• Harvard University

• Smithsonian Astrophysical Observatory

• Australian National Univ.

• Australian Astronomy Lim.

• Texas A&M University

• University of Texas, Austin• University of Arizona

• + …OTHERS TBD (Korean!)

GMT Design

Alt-az structure

Seven 8.4-m primary mirrors

• Cast borosilicate honeycomb

• 25.3-m enclosed diameter

• 24-m diffraction equivalent

• 21.5-m equivalent aperture

3.2-m adaptive Gregorian secondary mirror

Instruments mount below M1 at the Gregorian focus

Conceptual Design Review: February, 2006 Strong endorsement of design / low risk / group involved

GMT Optical Design• Primary Mirror

– D1 = 25.3 meter– R1 = 36.0 meters– K = -0.9983– f/0.7 primary mirror overall

• Gregorian secondary mirror– D2 = 3.2 meter– R2 = 4.2 meter– K2 = -0.7109– Segments aligned with primary

mirrors

• Combined Aplanatic Gregorian focus– f/8.2 final focal ratio– Field of view: 24 - 30 arc-

min. – BFD = 5.5 meters– M2 conjugate = 160 m above M1

GMT Structure

Design goal: Compact, stiff Structure

Low wind cross-section

Maximize modal performance

Minimum swing radius -> cost

Model parameters Analysis includes telescope structure,

optics, & instrument load

Height = 36.1 meters

Moving mass = 991 metric tons

Lowest vibration mode = 5.1 Hz

Segmented Gregorian Secondary Mirrors

Adaptive secondary (ASM):

Technology developed for MMT & LBT

~672 actuators per segment

~4700 actuators total

Capacitive position sensors.

In-telescope calibration source.

Fast-steering secondary (FSM):

Seven 1.06 m segments aligned with primary mirror segments

Fast tip-tilt actuators

GMT Enclosure Concept

Enclosure Structure

M3 Engineering

Height: 60 m

Diameter: 54 m

Structure design & cost study complete 12/04

Thermal & flow studies

On-site Facilities design

October 4, 2007___________________________________________________________

Giant Magellan Telescope Site SelectedThe Giant Magellan Telescope (GMT) Consortium announces

that the GMT will be constructed at Cerro Las Campanas, Chile.

Magellan (Manqui) Campanas Pk.Alcaino Pk.

Ridge (Manquis)

The Site


K-GMT Plan

• Project Period : 2009-2018 (10 yrs)• Budget : 97M USD

– 10% of GMT : 60M$– Science, Prerunner Instrument, K-GMT Office

• Job opened : ~32 (10 Engineers inc.)


Korean Institutes & Companies

•Adaptive Optics–Laser Guide Star–LTAO, GLAO, ExAO

•Steering Secondary•Telescope Structure•Dome Enclosure

KNU ( 공주대 )

KRISS ( 표준연구원 )

(KIMM 기계연구원 )

Dusan Infra Core( 두산인프라코아 )

…

•Science•Instruments

– Optical Design– Integration & Test– Fabrication

Korean Astronomical SocietyKASI, Univ.

KBSI ( 기초연 )


Giant Magellan Telescope

Proposed 1st GenerationInstruments


GMT Science Requirements

1. High Level Science Goals

2. Definition of the Telescope and Related Facilities

3. Site Requirements

4. First Generation Instrument Specifications

5. Adaptive Optics Capabilities

6. Support Facilities

7. Operational Requirements

8. Image Size and Wave-Front Requirements


High High

LevelLevel

SciencScience e

GoalsGoals


First Generation Instrument CandidatesInstrument (m) Resolution FOV Modes

Visible WF MOS 0.4 - 1.0 500-5000 60-150 � MOS, Imager

NIR MOS 0.9 - 2.5 1500-5000 25-100 � MOS/IFU

Imager

Visible Echelle 0.3 - 1.0 20K - 100K 20 Single Object Fiber feed

NIR Echelle 1 - 5 50K-150K 30 Single Object

MIR AO Imager 3 - 25 5-3000 2 x 2 Coronagraph Nulling int.

NIR AO Imager 1 - 2.5 5-5000 30 ``Wide-field’’ & high definition modes

NIR IFU` 1 - 2.5 3000-5000 3” LTAO, MCAO(?)


GMT InstrumentsInstrument P.I. Mode Port

1. Visible-band Multi-object Spectrograph

S. Shectman

(Carnegie)

Natural seeing, GLAO

Gregorian

2. High Resolution Visible Spectrograph

P. McQueen Natural seeing Folded port

3. Near-IR Multi-Object Spectrograph

D. Fabricant

(SAO)

Natural Seeing, GLAO

Gregorian

4. Near-IR Extreme AO Imager

L. Close

(U. Arizona)

ExAO Folded port

5. Near-IR High Resolution Spectrometers

D. Jaffe

(U. Texas Austin)

Natural seeing, LTAO

Folded port

6. Mid-IR AO Imager & Spectrograph

P. Hinz

(U. Arizona)

LTAO Folded port


Instrument Match to Science Goals# Science Area Sub-Area Instruments Notes1 Exoplanets Direct imaging 6, 4 ExAO, Nulling

Disks scattering 6, 4Disk emission 4, 6 mid-IRRadial vel. surveys 3, 5

2 Solar System KBOs 1, 6Comets & Moons 3, 5, 4

3 Star Formation Embedded clusters 6, 4Proper motions 1 GLAO criticalCrowded fields 6, 2, 1Mass ratios 6, 3, 5

4 Stellar Pops Stellar abundances 3, 5Pop. Studies 1, 6, 3

5 Black Holes AGN Environments 1, 6, 2 IFU,TF ModesVelocity structures 6, 1 IFU Mode

6 Dark Energy SNe monitoring 6, 1, 2SNe physics 1, 2 Polarim. mode

7 Galaxy Ass. Stellar mass density 1, 2Internal dynamics 2, 6

8 First Light IGM studies 1, 3, 2, 5First Galaxies 1, 2, 6


Gregorian Instrument Mounting

Large survey instruments mount below

AO instruments - always “hot” - above


GMT Instrument Platform (IP)

RotatorGLAO Guider

Folded portinstruments

Gregorianinstruments

capacity6.4 m Dia.7.6 m high

25 ton

Optical MOS

Near-IR MOS

Mid-IR Spectrograh

Echelle

NIR AO imager

NIR Echelle

Small-intermediate sized intstruments

Rapid exchange


Multiple Instruments at Gregorian Focus

GMACSNIRMOS

removed


First Generation Instrument Candidates

1. Visible Multi-Object Spectrograph

Four-Arm Double Spectrograph

18’ x 9’ FOV - VPH grisms - Transmission optics

R ~ 3500 (red) & ~ 1200 (blue) primary mode

higher and low R modes available

Multiplexing factor ~ 500 - 1000 depending on mode


GMACS- Visible band MOS

Shectman, et. al.


GMACS- Visible band MOS



3. Near-IR Multi-Object Spectrograph

Refractive Optics - Collimator-Camera Design

7’ x 7’ Imaging Field - 5’ x 7’ Spectroscopic

R = 3200 & R = 1500 modes

10k x 6k detector mosaic

(80) < 0.15” - 0.067” pixels

IFU mode under development


GMT NIRMOSInstrument Mounting

Flange

Support Roller Interface Ring

Fabricant, et. al.


GMT NIRMOS

Instrument Platform

Available Cassegrain Instrument Volume

6.35 m

5.2 m

7.62 m



5. High Resolution Near-IR Spectrograph

Two Channels: 1 - 2.5m Natural Seeing or AO

3 - 5m Diffraction-Limited

Silicon Immersion gratings

R ~ 25-100k (JHK) & 100-150K (L&M)

4k x 4k HgCdTe FPAs


Near-IR High-resolution Spectrometer

Short wavelength module: J, K, H

Jaffe, et. al.


K-GMT Instrument Strategy


Basic Strategy

• Base on the our experience in optical/IR instrument• Join ASAP

– Design & Integration/Test Phase are most important to us– More chance to find our role at early stage

• Step 2 : Magellan/MMT instrument– To increase our experience– To get Telescope time like US TSIP program

• Cooperation with Korean Institutes and companies


Our Experience in Optical/IR

1970- : SOAO1980- : 4ch Photometer1996 : BOAO1998 : 2K CCD2005 : BOES2007 : KASINICS

Multi-Object Optical Spectrograph (GMACS)

and/orNear IR Imager/Spectrograph (NIRMOS)

and/orNear-IR High Resolution Spectrometer (GMTNIRS)


Joint ASAP : Timeline


기기개발 로드맵기기개발 로드맵

국내기기

WIFIS(4m)

MMT관측기기

GMT관측기기

관측기기독자개발능력확보

관측기기독자개발능력확보


K-GMT Prerunner Instruments


On-going Project : WIFIS

WIFIS : Wide Integral-Field IR SpectrographImage slicers-based IFU, FISICA (Florida Image Slicer for Infrared Cosmology & A

strophysics)

R ~ 5,000; FOV = 13”X33” (at f/15 4m), each but whole J, H, or K band

International collaboration :

University of Toronto (Dae-Sik Moon) – design, construction, etc.

University of Florida (Stephen S. Eikenberry) - FISICA

KASI team – Warm Electronics, Part of Optical Design

Expected first light : 2011

- 2007 - 08 Optical Design, Electronics

- 2009 Opto-Mechanical Design & Fab.

- 3.6m CFHT, 4m KPNO, 5m Paloma or 10.4m GTC


- 태양계 천체의 연구

- 별 탄생 영역의 관측을 통한 별 형성과정 연구

- 원시행성계 원반 , 행성을 보유한 별 등의 관측을 통한 행성계 형성과정 연구

- 성협 , 거대분자운 , 조 기형 별 , 밀집 HII 영역 , 우리은하 중심부와 bulge 등 성간소광이심한 영역의 관측연구

- 우리은하 산개성단 및 구상성단의관측을 통한 성단 및 은하의 형성 , 구조와 진화 연구

- 외부은하의 성단 , 행성상성운 , HII 영역 및 항성종족 연구

- 활동성은하핵 , Starburst 은하 , 초신성 , 검은구멍 , X 선 쌍성 , 퀘이사 등의 관측 연구

- 은하단의 관측을 통한 은하단의 형성 , 구조와 진화 및 암흑물질 연구

- 은하간 물질의 화학조성 연구

WIFIS Science


Univ. of Florida, KPNO 4m

FOV(4m f/15)

Resolution Band

Flamingo 13”X33” 1,500 JH or HK

WIFIS 13”X33” 5,000 J, H, or K

WIFIS vs. Flamingo


x

y

Datacube

ImageImageslicerslicer

slitMicro-mirrors

FibreFibrearrayarray

slitFibres

TelescopeTelescopefocusfocus

SpectrographSpectrographinputinput

Lensletarray

SpectrographSpectrographoutputoutput

Pupilimagery

Micro-Micro-slicerslicer

Anamo-rphism

Centre for Advanced Centre for Advanced InstrumentationInstrumentation

Main techniques of IFS

Slicers retainSlicers retainspatial informationspatial informationalong slicealong slice


Instrument

Telescope

Spectral Res. R

Sp. range†

Field of View

Spacial Resolution‡ IFU type

FISICA+FLAMINGO

KPNO 4m ~1300 ≤ 1.2㎛ 16″×33″ 0.8″×0.6″image slice

GNIRS-IFUGemini

S.~1,700 ≤ 1.5㎛ 3.2″×4.

8″

image slice

" " ~6,000 ≤ 0.4㎛ 3.2″×4.8″

image slice

NIFSGemini

N.~5300 ≤ 0.4㎛ 3.0″×3.

0″0.1″×0.04

″image slice

CIRPASSGemini

S.~3000 ≤ 0.2㎛ 10″×5″

0.35″ or 0.26″

lenslet + fiber

UIST-IFU UKIRT ≤4,000 ≤ 0.3㎛ 3.3″×6.0″

0.24″×0.12″

image slice

† 수록된 파장폭은 K 밴드 부근에서 값이다 . 짧은 파장 J, H 밴드에서는 더 좁아진다 .‡ 공간분해능은 조각나누기 거울 좁은 쪽 폭 × 2 픽셀 슬릿 폭이다 .

IFU IR Spectrograph


Step 2 : MMT/etc Instruments project

Binospec IGNIRS HERMES

Science Large scale Structure & Galaxy Evol

Star & Planet Formation

Our Galaxy structure

Chemical Tagging

사업기간 4 년 (2011) 4 년 (2011) <4 년

부착망원경 MMT NOAO Tel (or IRTF)

AAT

한국참여지분 >3.9MUSD

( 인건비 포함 )

1.2M~0.2M

( 재료비만 )

1M

( 정확하지 않음 )

한국참여형태 기술인력 파견 , 기술습득

한국주도 혹은공동개발

공동개발파트제작제공


감사합니다 .

k-gmt prerunner instruments – m-y chun – sdss-ksg 2008 feb. 19 1 k-giant prerunner instruments...

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