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K-Giant Prerunner Instruments. 2008. Feb. 19. SDSS-KSG 워 크샵 천무영. Giant Magellan Telescope Project. GMT Institutions. Carnegie Observatories Harvard University Smithsonian Astrophysical Observatory Australian National Univ. Australian Astronomy Lim. Texas A&M University

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K giant prerunner instruments

K-Giant Prerunner Instruments

2008. Feb. 19.SDSS-KSG 워크샵천무영



Gmt institutions
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
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
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
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
Segmented Gregorian Secondary Mirrors

  • Fast-steering secondary (FSM):

    • Seven 1.06 m segments aligned with primary mirror segments

    • Fast tip-tilt actuators

Adaptive secondary (ASM):

Technology developed for MMT & LBT

~672 actuators per segment

~4700 actuators total

Capacitive position sensors.

In-telescope calibration source.



Enclosure Structure

Height: 60 m

Diameter: 54 m

Structure design & cost study complete 12/04

Thermal & flow studies

On-site Facilities design

M3 Engineering


The site

Magellan (Manqui)

Campanas Pk.

Alcaino Pk.

Ridge (Manquis)

The Site

October 4, 2007

___________________________________________________________

Giant Magellan Telescope Site Selected

The Giant Magellan Telescope (GMT) Consortium announces

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


K gmt plan
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)

Korean Institutes & Companies

  • Science

  • Instruments

    • Optical Design

    • Integration & Test

    • Fabrication

  • Korean Astronomical Society

  • KASI, Univ.

  • KBSI (기초연)


Giant magellan telescope proposed 1 st generation instruments
Giant Magellan TelescopeProposed 1st GenerationInstruments


Gmt science requirements
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

Level

Science

Goals





Gregorian instrument mounting
Gregorian Instrument Mounting

Large survey instruments mount below

AO instruments - always “hot” - above


Gmt instrument platform ip
GMT Instrument Platform (IP)

Rotator

GLAO Guider

Folded port

instruments

Echelle

NIR AO imager

NIR Echelle

Small-intermediate sized intstruments

Rapid exchange

Gregorian

instruments

capacity

6.4 m Dia.

7.6 m high

25 ton

Optical MOS

Near-IR MOS

Mid-IR Spectrograh



First generation instrument candidates1
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
GMACS- Visible band MOS

Shectman, et. al.



First generation instrument candidates2
First Generation Instrument Candidates

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

q(80) < 0.15” - 0.067” pixels

IFU mode under development


Gmt nirmos

Instrument Mounting

Flange

Support Roller Interface Ring

GMT NIRMOS

Fabricant, et. al.


Gmt nirmos1

Instrument Platform

5.2 m

7.62 m

Available Cassegrain

Instrument Volume

6.35 m

GMT NIRMOS


First generation instrument candidates3
First Generation Instrument Candidates

5. High Resolution Near-IR Spectrograph

Two Channels: 1 - 2.5mm Natural Seeing or AO

3 - 5mm Diffraction-Limited

Silicon Immersion gratings

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

4k x 4k HgCdTe FPAs


Near ir high resolution spectrometer
Near-IR High-resolution Spectrometer

Short wavelength module: J, K, H

Jaffe, et. al.



Basic 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- : SOAO

1980- : 4ch Photometer

1996 : BOAO

1998 : 2K CCD

2005 : BOES

2007 : KASINICS

Multi-Object Optical Spectrograph

(GMACS)

and/or

Near IR Imager/Spectrograph

(NIRMOS)

and/or

Near-IR High Resolution Spectrometer (GMTNIRS)

Our Experience in Optical/IR



기기개발 로드맵

국내기기

관측기기독자개발능력확보

WIFIS(4m)

MMT

관측기기

GMT관측기기



On going project wifis
On-going Project : WIFIS

  • WIFIS : Wide Integral-Field IR Spectrograph

  • Image slicers-based IFU, FISICA (Florida Image Slicer for Infrared Cosmology & Astrophysics)

  • 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


Wifis science
WIFIS Science

- 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, X선 쌍성, 퀘이사 등의 관측 연구

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

- 은하간 물질의 화학조성 연구


Wifis vs flamingo
WIFIS vs. Flamingo

Univ. of Florida, KPNO 4m

IFU Module

FISICA +

IR Spectrograph

WIFIS

IR Spectrograph

Flamingo


Main techniques of ifs

Telescope

focus

Spectrograph

input

Spectrograph

output

Pupil

imagery

Lenslet

array

Fibres

slit

Datacube

Fibre

array

Image

slicer

Micro-

mirrors

slit

y

x

Anamo-

rphism

Micro-

slicer

Slicers retain

spatial information

along slice

Main techniques of IFS

Centre for Advanced Instrumentation





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