Characterizing Exoplanets: The Challenge

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 ~ 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)

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 ~ 105 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 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

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

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

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

13. 0.1 AU ~1000 K 1 AU ~200 K 10 AU ~50 K H2 UV, NIR, MIR H2O ro-vib OH Dv=1 CO Dv=1 CO Dv=2 Planet Formation Environments Studying gas in disks: (thermal) Study gas dissipation timescale: constrains pathways for giant planet formation, terrestrial planet architectures

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 (106 - 107 contrast)

15. 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.

16. U Colorado HROS Concept

17. PFI Science Missions

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. 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

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)