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Future of the GMT

GMT2010: Opening New Frontiers with the Giant Magellan Telescope. Future of the GMT. Centre for Astrophysics and Supercomputing. Warrick Couch Swinburne University. Purpose?. “the GMT project is anticipated to bring a quantum jump in the development of Korean astronomy .”.

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Future of the GMT

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  1. GMT2010: Opening New Frontiers with the Giant Magellan Telescope Future of the GMT Centre for Astrophysics and Supercomputing Warrick Couch Swinburne University

  2. Purpose? “the GMT project is anticipated to bring a quantum jump in the development of Korean astronomy.” “The goal of this workshop is to review the current status of the GMT project and to discuss sciences, instruments and some of the technical challenges for the GMT.”

  3. SCIENCE – no shortage of ideas and drivers for GMT, some of which will be transformational! • Disks and planets • debris disks (Song); transitional systems (Lyo) • Stars and the ISM • stars with planets (Kang); ISM around SNRs/YSOs (Shinn); SNR shock filaments (Lee) Plus 11+ posters in most of these areas! • Galaxies, AGN, Cosmology • LSS/galaxy evoln (Park); MBH/galaxyevoln(Woo); massive galaxy formation (Yi); Lyα blobs (Yang); N-F cosmol(M-G Lee, An); LRSI (J Lee); glob clusters (Y-W Lee, J-W Lee); cluster gal evoln (Lee, Kim) • First objects in the universe • QSOs as probes (Im); 1st stars relic signature (Ahn); testing expansion using LSS topology (Rossi)

  4. SCIENCE – important synergies GMT will have with other major telescope facilities • JWST (Mark Clampin) [launch ≥ 2014] • Will win hands down on broad-band imaging over NIR and MIR regions • GMT wins in terms of spatial resolution (@DL) and sensitivity for R>1000 NIR spectroscopy • ALMA (NagayoshiOhashi) [2012] • Molecular gas content and thermal dust emission measurements of importance to ALL science areas/targets of interest to GMT • Diffraction-limited spatial resolution of GMT well matched to that of ALMA (~20mas in K) GMT’s southern hemisphere location will also mean strong synergies with LSST and SKA

  5. INSTRUMENTS – the ‘vehicles’ for realizing our scientific aspirations and whose capabilities are determined accordingly! • GMACS (DePoy) • NIRMOS (Fabricant) • GMTNIRS (Jaffe) • GMTIFS (McGregor) GLAO AO AO • G-CLEF (R=20,000-150,000 optical spec) • TIGER (Mid-IR imager with coronagraph) • MANIFEST (MANy Instrument FibrESysTem) AO Hard choices will have to be made – essential the GMT partnership is very clear on its scientific priorities & the best instrument choices given GMT design & competition

  6. TECHNICAL CHALLENGES Two key areas: (1)Mirror design and fabrication • M1 (7 x 8.4m) – can we produce off-axis segments; can we do it fast enough? • M2 (7 x 1.1m ASM’s) – build and integrate to work in concert with M1 segments? (2)Adaptive Optics (NGS, LTAO, MCAO, ExAO) • Obvious complexity! • Segment piston error – phase of the incoming wavefront cannot be measured between M1 segments

  7. CAUSE FOR OPTIMISM “Ground‐layer AO with an adaptive secondary is now a demonstrated image sharpening technique with enormously broad application.” – M. Hart

  8. The future of GMT – other challenges ahead

  9. Many key challenges & decision points during this period (from Pat McCarthy)

  10. Main challenges & decisions looming: • Primary mirror segment production • Need to produce remaining 6 segments in 8 yrs (avg: 1 per 16 months) to make mid-2019 deadline • Instrument selection • We cannot have them all; will need to down-select 2-3 as ‘first light’ instruments – which ones??? • Preliminary Design Review • Revised and more accurate construction costing • Outstanding risks yet to be retired?

  11. Main challenges & decisions looming: • Funding • 35% of funding required for GMT construction raised; but remaining 65% still to be found • What fraction of total construction budget needs to be raised before construction can begin? • Cost/danger of sustaining/losing ‘marching army’ • Partners • GMT partnership 85% subscribed • Intentions of US NSF re GMT involvement? • Implications of US Decadal Survey (ASTRO2010)?

  12. Key Members or The Project Team Matt Johns Project Manager Steve Shectman Project Scientist George Jacoby Instrumentation Scientist Steve Gunnels Lead Mechanical Engineer Antonin Bouchez AO Scientist Steven Dolmseth CFO Jose Filgueira Lead Controls Engineer Michael Ward Lead Systems Engineer 15

  13. GMT Adaptive Optics Team Antonin Bouchez GMT AO Scientist Palomar AO System Olivier Guyon Subaru AO Lead Phil Hinz LBTI PI, MMT AO Michael Hart MMT ASM, GLAO Marcos Van Dam AO Consultant

  14. Harvard Carnegie SAO KASI U. Arizona U. Texas Austin Texas A&M ANU LCO GMT Workshops GMT Institutions ??? (2010) (2008) AAL (2010)

  15. Finally, some thanks are in order: • MyungGyoon Lee for chairing the SOC • MyungshinIm(Chair) and his LOC team: Sang ChulKim, Young-SooKim, Jeong-EunLee, Soojong Pak, Jong-Hak Woo • Seoul National University and KASI for sponsoring the meeting • Seoul National University for hosting the meeting

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