Ben R. Oppenheimer, Sasha Hinkley, Anand Sivaramakrishnan, Remi Soummer, Douglas Brenner

1. PROJECT 1640 AN ANCILLARY OF Ben R. Oppenheimer, Sasha Hinkley, Anand Sivaramakrishnan, Remi Soummer, Douglas Brenner Ian Parry, David King, Steve Medlen http://lyot.org

2. Digital Universe: http://haydenplanetarium.org

3. Giants to scale Planets are complex Vogt-Russell Theorem: “mass and chemical composition are sufficient to determine the structure, evolution and outward appearance of a star completely” Planets have a diversity possibly unmatched in astronomy, and the theorem does not apply The onset of complexity perhaps begins in the brown dwarf mass range where age is needed as well. In coolest or lowest mass BDs, more complexity: The chemistry and SEDs are drastically affected by minor changes in composition, mass, age Terrestrial Planets to scale A few simple parameters are insufficient to determine a planet’s salient features.

4. 3.6 m telescope atop Haleakela (Maui) • 941 actuator AO system • 80-90% Strehl at H-Band • Optimized, diffraction-limited coronagraph • 30 stars observed (1 candidate planet, 7 BDs, 3 disks) • Differential Polarimeter working • Integral Field Unit being built now

5. Planet and Brown Dwarf Sensitivity Lyot Project Discovery Space Known but unseen exoplanets (Marcy et al. 2003)

6. Some Nearby Star H-Band S ~ 80-90% H-Band 15 minute exp. Oppenheimer et al. in prep. Weird colors (i, z, J, H, K) Companionship confirmed Speckles are the bane of any exoplanet imager, even in space!

7. Dynamic Current Performance Dynamic Range Vega Companion Mass limits Polarimetry Speckle subtraction Hinkley et al. 2006, astro-ph/0609337

8. HR4796 Oppenheimer et al., in prep.

9. Project 1640: Integral Field UnitSeeing through the speckles • Data Cube Movie • 10 nm Steps • S ~ 90% • = 1.6 m (1.0 at left) Planet has flat spectrum AO Performance matched to current AEOS performance

10. Optics R ~ 30-100 lenslet-based IFU J-H band (1-1.85 µm) 4” FOV (200x200 spatial pixels) First Light Jan 2008 Lenslet Array HAWAII-II Array Prism ~0.5 m Dewar is Identical to PHARO’s

11. Planet and Brown Dwarf Sensitivity PALM3000 + P1640 Discovery Space Known but unseen exoplanets (Marcy et al. 2003)

12. Project 1640 Passed CDR Design Review included 4 external people: Jamie Lloyd (Cornell), James Larkin (UCLA), David Schiminovich (Columbia) Russ Makidon (STScI) Recommendation: “collaboration with the Palomar Observatory should be sought immediatelyto put the team and Palomar at the forefront of high contrast science” July at AMNH Concept: Bring 1640 to 200” put it and a small version of Lyot behind the 3000 actuator AO system Fully funded ($1.8M)

13. P1640 with PALM3000 Unique capability for years to come Gemini Planet Imager and VLT’s SPHERE slated for late 2010 and both are in the south, and perhaps only marginally more sensitive Hundreds of planets, circumstellar disk chemistry, disk evolution PALAO (prior to upgrade): 1-2 magnitude improvement over AEOS but much fainter stars are accessible LGS: Galaxies Solar System science (eg Kuiper belt moon spectroscopy) Young stars Debris disk science - spatially resolved chemistry M-dwarf companions Evolved star astrophysics We have the money, the people and an instrument. Palomar is the best place in the world suited to do this work

14. Ten Years of Coronagraphy A Decade of Coronagraphy Part of Palomar’s Heritage is Cutting-dege Coronagraphy