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K-Giant Prerunner Instruments

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

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  1. K-Giant Prerunner Instruments 2008. Feb. 19.SDSS-KSG 워크샵천무영

  2. Giant Magellan TelescopeProject

  3. 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!)

  4. 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

  5. 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

  6. 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

  7. 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.

  8. GMT Enclosure Concept

  9. Enclosure Structure Height: 60 m Diameter: 54 m Structure design & cost study complete 12/04 Thermal & flow studies On-site Facilities design M3 Engineering

  10. 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.

  11. 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.)

  12. 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)

  13. Giant Magellan TelescopeProposed 1st GenerationInstruments

  14. 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

  15. High Level Science Goals

  16. First Generation Instrument Candidates

  17. GMT Instruments

  18. Instrument Match to Science Goals

  19. Gregorian Instrument Mounting Large survey instruments mount below AO instruments - always “hot” - above

  20. 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

  21. Multiple Instruments at Gregorian Focus removed NIRMOS GMACS

  22. 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

  23. GMACS- Visible band MOS Shectman, et. al.

  24. GMACS- Visible band MOS

  25. 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

  26. Instrument Mounting Flange Support Roller Interface Ring GMT NIRMOS Fabricant, et. al.

  27. Instrument Platform 5.2 m 7.62 m Available Cassegrain Instrument Volume 6.35 m GMT NIRMOS

  28. 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

  29. Near-IR High-resolution Spectrometer Short wavelength module: J, K, H Jaffe, et. al.

  30. K-GMT Instrument Strategy

  31. 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

  32. 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

  33. Joint ASAP : Timeline

  34. 기기개발 로드맵 국내기기 관측기기독자개발능력확보 WIFIS(4m) MMT 관측기기 GMT관측기기

  35. K-GMT Prerunner Instruments

  36. 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

  37. 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

  38. WIFIS vs. Flamingo Univ. of Florida, KPNO 4m IFU Module FISICA + IR Spectrograph WIFIS IR Spectrograph Flamingo

  39. 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

  40. IFU IR Spectrograph

  41. Step 2 : MMT/etc Instruments project

  42. 감사합니다.

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