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K-Giant Prerunner Instruments
2008. Feb. 19.
SDSS-KSG 워크샵
천무영
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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Giant Magellan Telescope
Project
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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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
•
•
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 Optical Design
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
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.
GMT Enclosure Concept
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)
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
• 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.)
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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Korean Institutes & Companies
•Adaptive Optics
–Laser Guide Star
–LTAO, GLAO, ExAO
•Steering Secondary
•Telescope Structure
•Dome Enclosure
•Science
•Instruments
– Optical Design
– Integration & Test
– Fabrication
KNU (공주대)
KRISS (표준연구원)
(KIMM 기계연구원)
Dusan Infra Core(두산인
프라코아)
Korean Astronomical Society
…
KASI, Univ.
KBSI (기초연)
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Giant Magellan Telescope
Proposed 1st Generation
Instruments
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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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
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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High
Level
Science
Goals
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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First Generation Instrument Candidates
(m)
Resolution
FOV
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
NIR IFU`
1 - 2.5
3000-5000
3”
Instrument
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
Modes
``Wide-field’’ &
high definition
modes
LTAO, MCAO(?)
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GMT Instruments
Instrument
P.I.
Mode
Port
1. Visible-band Multiobject Spectrograph
S. Shectman
(Carnegie)
Natural seeing,
GLAO
Gregorian
2. High Resolution
Visible Spectrograph
P. McQueen
Natural seeing
Folded port
D. Fabricant
(SAO)
Natural Seeing,
GLAO
Gregorian
L. Close
(U. Arizona)
ExAO
Folded port
D. Jaffe
(U. Texas Austin)
Natural seeing,
LTAO
Folded port
P. Hinz
(U. Arizona)
LTAO
Folded port
3. Near-IR Multi-Object
Spectrograph
4.
Near-IR Extreme
AO Imager
5. Near-IR High
Resolution Spectrometers
6.
Mid-IR AO Imager
& Spectrograph
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Instrument Match to Science Goals
#
1
Science Area
Exopl anets
2
Solar System
3
Star Formation
4
Stell ar Pops
5
Black Holes
6
Dark Energy
7
Galaxy Ass.
8
First Li ght
Sub-Area
Dir ect im aging
Disks scattering
Disk emission
Radial ve l. survey s
KBOs
Comets & Moons
Embedded clusters
Proper motion s
Crowded fie lds
Mass ratios
Stell ar abundan ces
Pop. Studi es
AGN Env ir onments
Velocit y structures
SNe moni toring
SNe phys ics
Stell ar mass dens it y
Internal dyna mi cs
IGM studies
First Galaxies
Instruments
6, 4
6, 4
4, 6
3, 5
1, 6
3, 5, 4
6, 4
1
6, 2, 1
6, 3, 5
3, 5
1, 6, 3
1, 6, 2
6, 1
6, 1, 2
1, 2
1, 2
2, 6
1, 3, 2, 5
1, 2, 6
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
Notes
ExAO, Nulli ng
mi d-IR
GLAO criti cal
IFU,TF Modes
IFU Mode
Polarim. m ode
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Gregorian Instrument Mounting
Large survey instruments mount below
AO instruments - always “hot” - above
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GMT Instrument Platform (IP)
Rotator
GLAO Guider
Folded port
instruments
Echelle
Small-intermediate
NIR AO imager
sized intstruments
NIR Echelle
Rapid exchange
Gregorian
instruments
capacity
Optical
MOS
6.4 m Dia.
Near-IR
MOS
7.6 m high
Mid-IR 25
Spectrograh
ton
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Multiple Instruments at Gregorian Focus
removed
NIRMOS
GMACS
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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
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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GMACS- Visible band MOS
Shectman, et. al.
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GMACS- Visible band MOS
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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
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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GMT NIRMOS
Instrument Mounting
Flange
Support Roller
Interface Ring
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
Fabricant, et. al.
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GMT NIRMOS
Instrument Platform
5.2 m
7.62 m
Available Cassegrain
Instrument Volume
6.35 m
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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First Generation Instrument Candidates
5. High Resolution Near-IR Spectrograph
Two Channels: 1 - 2.5m
3 - 5m
Natural Seeing or AO
Diffraction-Limited
Silicon Immersion gratings
R ~ 25-100k (JHK) & 100-150K (L&M)
4k x 4k HgCdTe FPAs
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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Near-IR High-resolution Spectrometer
Short wavelength module: J, K, H
tertiary
FPA
primary
secondary
cross
disperser
echelle
fold
slit
collimator
Jaffe, et. al.
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
200.00 mm
Scale: 1/8
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K-GMT Instrument Strategy
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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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
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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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)
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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Joint ASAP : Timeline
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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기기개발 로드맵
국내기기
관측기기
독자개발
능력확보
WIFIS
(4m)
MMT
관측기기
GMT
관측기기
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K-GMT Prerunner Instruments
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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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
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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
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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WIFIS vs. Flamingo
Univ. of Florida, KPNO 4m
FOV
(4m f/15)
Flamingo 13”X33”
Resolution Band
WIFIS
5,000
13”X33”
1,500
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
JH or
HK
J, H, or
K
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Main techniques of IFS
Telescope
focus
Lenslet
array
Fibre
array
Image
slicer
Microslicer
Centre for Advanced
Spectrograph
input
Spectrograph
output
Pupil
imagery
slit
Datacube
Fibres
Micromirrors
slit
y
x

Anamorphism
K-GMT
Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
Instrumentation
Slicers retain
spatial information
along slice
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IFU IR Spectrograph
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-IFU
Gemini S.
~1,700
≤ 1.5㎛
3.2″×4.8″
image slice
"
"
~6,000
≤ 0.4㎛
3.2″×4.8″
image slice
NIFS
Gemini N.
~5300
≤ 0.4㎛
3.0″×3.0″ 0.1″×0.04″
image slice
CIRPASS
Gemini S.
~3000
≤ 0.2㎛
UIST-IFU
UKIRT
≤4,000
≤ 0.3㎛
10″×5″
0.35″ or
0.26″
lenslet +
fiber
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.
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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Step 2 : MMT/etc Instruments project
Binospec
IGNIRS
HERMES
Science
Large scale
Structure &
Galaxy Evol
Star & Planet
Formation
Our Galaxy
structure
Chemical Tagging
사업기간
4년(2011)
4년(2011)
<4년
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 혹은
공동개발
공동개발
파트제작제공
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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감사합니다.
K-GMT Prerunner Instruments – M-Y Chun – SDSS-KSG 2008 Feb. 19
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