1. Characterizing Exoplanets: The Challenge

2. 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 ~ 10 7 Detection of lower mass planets is possible, but star suppression must exceed 10 8 –Characterization via spectroscopy not possible GSMT will detect ‘warm Jupiters’ around t < 10 Myr stars in nearby star-forming regions (75-150 pc)

3. ELT Projects

4. 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

5. 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

6. 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?

7. TMT Reference Design 30-m segmented primary f/1 Gregorian 10’FOV, kilo-slit MOS Deployable IFUs + imager diffraction-limited 0.05” pixel R ~ 10 5 MIR spectrograph ExAO coronagraph

8. 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

9. 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  m; 5  m 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  m; 5  m goal) MIRES - R ~ 10 5 spectrograph (5-30  m) WFOS - kiloslit wide-field optical spectrograph

10. Lenslet Optics AO Focus Reimaging Collimators Filters Reimaging Cameras Fold Mirror & Lenslet Array Spectrograph Collimator Mirrors (TMA) Grating Fold Mirror Spectrograph Camera Mirrors (TMA) Detector IRIS: UCLA led collaboration

11. Image Slicer Fiber Bundle Lenslet Array Focal Plane Feed to Spectrograph Detector 1 2 3 4 Deconstructing Forming Galaxies at 7 mas resolution

12. MIRES (UH; NOAO; UCD; Texas) Echelon is ~1 m long

13. Planet Formation Environments 0.1 AU ~1000 K 1 AU ~200 K 10 AU ~50 K H 2 O ro-vib CO  v=2 CO  v=1 H 2 UV, NIR, MIR OH  v=1 Study gas dissipation timescale: constrains pathways for giant planet formation, terrestrial planet architectures Studying gas in disks: (thermal)

14. 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 (10 6 - 10 7 contrast)

15. Metal-poor Stars with HROS 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. HROS spectra of metal-poor stars

16. U Colorado HROS Concept

17. PFI Science Missions Science roleStar H magnitude DistanceAngular separation Contrast Very young planetary systems (1-10 Myr) 8-1150-150 pc0.04-0.1” (5 AU) 10 -6 Planetary census5-710-30 pc>0.05” (1 AU @ 20 pc) 10 -8 Planetary R=1000 spectroscopy 5-810-50 pc>0.1”10 -7 Circumstellar debris and zodiacal dust 5-810-50 pc>0.05” (0.5 AU@10 pc) polarimetry

18. 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

19. Site Evaluation

20. 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

21. 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

22. 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

23. Weather Station

24. Combining MASS + DIMM Results Free atmosphere seeing steady at ~ 0.25” for 4 nights

25. Advancing US ELT Efforts

26. AURA goals: –Ensure availability of ELT(s) early in the JWST era –Ensure broad community access –Provide a community voice in shaping ELT designs

27. 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

28. 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

29. 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

30. 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; opto- mechanical design Design MIRES (UH-NOAO collaboration)