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Characterizing Exoplanets: The Challenge GSMT Potential • GSMT will detect & classify Jovian mass planets, from ‘roasters’ to ‘old, cold’ Jupiters located at ~ 5AU for stars at d < 10 pc • Via photometry (R ~10) and low resolution spectroscopy (R ~200) • Requires star suppression ~ 107 • Detection of lower mass planets is possible, but star suppression must exceed 108 – Characterization via spectroscopy not possible • GSMT will detect ‘warm Jupiters’ around t < 10 Myr stars in nearby star-forming regions (75-150 pc) ELT Projects ESO OWL 100-m Concept • 100m segmented primary • Spherical segments • NGS AO • Find exo-earths • Stellar populations to Virgo • Design studies underway • Major funding after ALMA Magellan 20 Concept • 7x8.4m primary at f/0.7 • Possible upgrade path to 20/20 • General purpose telescope • wide FOV feeding MOS • NGS AO • MCAO • ExAO planet finder • Complete by 2014 • Partners: Carnegie, Arizona, CfA, MIT, Michigan, Texas, Texas A & M 20-20 Concept • 7x8.4m primary at f/0.7 • 100-m baseline • Detection of exo-earths • Other high contrast scenes • Magellan 20 + other partners? TMT Reference Design • 30-m segmented primary • f/1 Gregorian • 10’FOV, kilo-slit MOS • Deployable IFUs + imager • diffraction-limited • 0.05” pixel • R ~ 105 MIR spectrograph • ExAO coronagraph TMT Status • Partnership formed • UC, Caltech, Canada, AURA • Reference design selected (Oct, 2004) • based on CELT, VLOT and NIO/GSMT concepts • Design and Development phase underway • $70M effort • Private funding committed (Moore Foundation) • Public funding authorized (Canada; CFI) • NSF funding (1/2 x $1M FY05; $2M FY06; ramp up in FY07) • Site evaluation underway • Conceptual Design Review: Spring, 2006 • Cost review: Fall, 2006 TMT First Light Instruments Instrumentation priorities; requirements set by TMT SAC – Includes one representative from the community; 2 planned • NFIRAOS - facility AO system delivering narrow-field AO images (1-2.5 mm; 5mm goal) – 7 LGS constellation; deliver Strehl 0.7 images at K over 10” • Upgrade to 30” FOV by adding DMs – Feeds IRIS; NIRES; WIRC (see below) • IRIS - IFU spectrograph/imager (1-2.5 mm; 5mm goal) • MIRES - R ~ 105 spectrograph (5-30 mm) • WFOS - kiloslit wide-field optical spectrograph IRIS: Fold Mirror & Lenslet Array UCLA led collaboration Lenslet Optics Filters Reimaging Cameras Grating Spectrograph Collimator Mirrors (TMA) Detector Fold Mirror Spectrograph Camera Mirrors (TMA) AO Focus Reimaging Collimators Deconstructing Forming Galaxies at 7 mas resolution Focal Plane 1 Image Slicer Fiber Bundle Lenslet Array 2 3 4 Feed to Spectrograph Detector MIRES (UH; NOAO; UCD; Texas) Echelon is ~1 m long Planet Formation Environments Studying gas in disks: H2 UV, NIR, MIR H2O ro-vib OH Dv=1 CO Dv=1 (thermal) CO Dv=2 0.1 AU ~1000 K 1 AU ~200 K Study gas dissipation timescale: constrains pathways for giant planet formation, terrestrial planet architectures 10 AU ~50 K TMT Gen II Instruments • HROS - R ~70,000 optical spectrograph • IRMOS - deployable IFU IR spectrograph • WIRC - wide-field IR camera (MCAO) • NIRES - near-IR Echelle (R ~ 70,000) • PFI - ExAO imager (106 - 107 contrast) Metal-poor Stars with HROS HROS spectra of metal-poor stars • The nucleosynthetic “fingerprints” of Pop III stars, and the rare-earth elements produced in SN explosions are best observed at visible wavelengths. • R>30,000 required for reliable measurements of abundances even for very metal-poor stars. • Need TMT to be able to push out to other galaxies in the Local Group. U Colorado HROS Concept PFI Science Missions Science role Star H Distance magnitude Angular separation Contrast Very young planetary systems (1-10 Myr) 8-11 50-150 pc 0.04-0.1” (5 AU) 10-6 Planetary census 5-7 10-30 pc >0.05” (1 AU @ 20 pc) 10-8 Planetary R=1000 spectroscopy 5-8 10-50 pc >0.1” 10-7 Circumstellar debris and zodiacal dust 5-8 10-50 pc >0.05” (0.5 AU@10 pc) polarimetry TMT Operations Model • Plan for queue and classical operation • Invest in end-to-end system that envisions – Data reduction by PI and teams – Extensive post-proprietary period mining of archives populated by well characterized data • Community participation via – Classical or queue PI-mode observing – Planning and executing Legacy surveys • Community input needed – Desired operations modes – Mechanism for carrying out precursor/planning observations Site Evaluation GSMT Site Evaluation • NIO is involved in testing multiple sites: – – – – Las Campanas Three Chilean Sites Mauna Kea ELT site San Pedro Martir • Status: – Remote sensing studies (cloud cover; water vapor) nearly complete • MK / US / Chile comparison to finish in August – CFD modeling of sites: good progress on first three sites – Weather stations deployed on several mountains – Multi-Aperture Scintillation Sensor (MASS) • Measure turbulence profile above site • In combination with DIMM, quantify contribution of ground-layer Remote Sensing Survey of Cloud Cover and PWV • Survey uses meteorological satellite images • Long time baseline • Well-defined methodology provides: – Photometric, spectroscopic, unsuitable conditions based on cloud cover – Precipitable water vapor above the sites • Dispassionate comparison thus possible • Areas studied: – Northern Chile – SW USA-Mexico – Mauna Kea – Chile comparison Computational Fluid Dynamics • Characterize wind flow allowed pre-selection of sites – Wind intensity – Turbulence characteristics – Down-wind wakes • Characterization of all candidate sites now completed Weather Station Combining MASS + DIMM Results Free atmosphere seeing steady at ~ 0.25” for 4 nights Advancing US ELT Efforts Advancing US ELT Efforts • AURA goals: – Ensure availability of ELT(s) early in the JWST era – Ensure broad community access – Provide a community voice in shaping ELT designs AURA’s Approach • Goal: – Advance the design of TMT and GMT so that performance, cost, schedule and risk of differing approaches can be assessed • Provide $17.5M for TMT partnership – NSF dollars leveraged 3:1 • Provide comparable funds for GMT – Include funds for instrument concepts; technology – Program will be open to the entire US community Investment in TMT • Responds directly to AASC recommendations • The community will receive observing time in proportion to the public investment • AURA is represented at all levels in the project – The community has a ‘seat at the table’ throughout the Design and Development Phase • TMT Partners committed to engaging the community – Involve US and Canadian communities in instrument design – Involve US community members in the TMT SAC Advantages of AURA’s Approach • Directly responsive to SWG recommendations – Will fund two ELT programs: GMT and TMT • US community is engaged in ELT efforts and will receive time in proportion to federal investment in all ELTs • Open dialog between projects benefits all and leaves open a ‘convergence path’ • Technology investment in ELT programs will result in significant gains for existing telescopes Initial NSF funds received ($1M for FY05; $3M in FY06) Ramp up in FY 07 NIO Roles • • • • • Design M2 and M3 support and control system Design Laser launch facility Manage site evaluation process Develop observatory requirements document Provide engineering support: CFD; optomechanical design • Design MIRES (UH-NOAO collaboration)