1. GSMT in Astro 2010 - An Astrobiology Perspective Michael R. Meyer The University of Arizona (with input from James Graham and Steve Strom)

2. My ELT: Required Capabilities  Aperture > 20 meter (resolution over light-gathering)! » Piecing the “confusion-limited” veil…  Diffraction-limited imaging from 1-25 microns. » To reach < 3 AU around nearest young stars.  Near-/Mid-IR spectral resolution: R=30,000/50,000. » Origins of the cold and slow…  Near-/Mid-IR Field of View: > 2 arcminutes. » Size of nearest rich star clusters.  Precision visible RV: R > 40,000 with 10 cm/sec stability? » Earth-mass planets in HZ around late-type stars.

3. Take Home Message: The GSMT…..  Will play a key role in understanding star formation, planet formation, and the pathways enabling chemistry of life.  Is extremely complementary to JWST and ALMA.  Will help frame science questions for next generation missions with astrobio relevance (space strategic mission concepts as well as flagship missions).  Technology development on ground-based facilities can enhance flight programs.  Can be a concept for the COMMUNITY to participate in the LBT, the TMT, the GMT, and more!

4.  What are the most common host stars for potentially habitable planetary systems?  How do elements evolve into complex organic molecules that could give rise to life?  Are planetary systems like our own common or rare in the Milky Way? The Origins of Stars, Planets, and Life…

5. GSMT can study Forming Protostars with HST Resolution in the Thermal IR OSCIR @ N-band UFL on 3.6m Andersen, Meyer, Oppenheimer, Dougados, and Carpenter (2006) ~1 arcmin diameter.

6. Stellar Initial Mass Function (Chabrier, 2003; Kroupa et al. 2001) No variations locally in stellar IMF (Meyer et al. 2000). Turnover below 0.3 Msun universal (Andersen et al. 2008)?

7. Extreme Star-Formation in NGC 604 in M 33 at 1 Mpc

8. MMT-AO Engineering PSF Simulated Trapezium Observations R(Sky Noise) = 1 Rc = 0.2 pc from Close et al. 2003. using Hillenbrand & Carpenter (2000). Hcomp(at Rc) < 24 mag R(sky noise) = 2.5 Rc = 0.5 pc R(Sky Noise) = 4 Rc = 0.8 pc R(Sky Noise) > 20 Rc = 4-5 pc Hcomp(at Rc) < 17.8 mag. Hcomp(at Rc) < 15.3 mags. Core Radius not resolved. 25 kpc50 kpc0.5 Mpc 5 kpc PSF 0.5 kpc The Trapezium on the Bleeding Edge: Sensitivity vs. Confusion...

9. Different Flavors of Planet Formation

10. Dynamics and Chemistry of Collapsing Protostars GSMT Resolution will be < 2.5 AU for 4  m of nearest targets at 50 parsecs (e.g. TW Hya).. Yorke & Bodenheimer (1999) Lahuis et al. (2006).

11. How does chemistry affect planet formation? Gail (2002); Cody & Sasselov (2005); Garaud & Lin (2007); Bond et al. (in prep) Image courtesy N. Gehrels (PSU)

12. Planet-forming Disks: Molecular Abundances vs. Radius Courtesy J. Najita & S. Strom (NOAO) See also Pontoppidan et al. (2008) DQ Tau: Carr, Mathieu & Najita (2001) Simulation

13. 13 Disk Imaging: Courtesy J. Graham  Gravitationally sculpted disks provide key evidence for exoplanets » Morphology of dust trapped in libration points provides key to masses an eccentricities of exoplanets » Surface brightness,color, phase function, and polarization indicates quantity composition and grain size distribution  Synergy with JWST, Herschel, & ALMA » Probe disjoint dust grain populations and constraints the particle size distribution Maness, Kalas & Graham 2008 10 µm Gemini/Michelle 1.6 µm Keck AO 1 mm CARMA — HD 32297

14. TMT.INS.PRE.06.014.DRF01 14 Detection of Doppler Planets? Median Known Doppler Planets GSMT can target exoplanets in reflected light 30-m 3 /D Gemini 3 /D  Median contrast & angular separation for current catalog of Doppler planets » Q = 2 x 10 -8 »  = 30 mas  3 /D = 33 mas @ H » GSMT with high- performance diffraction suppression can detect Doppler planets

15. Background star; equivalent in brightness to a planet of ~5MJ. Planet Searches with MMT/CLIO A. Heinze, P. Hinz (PI), S. Sivanandam, M. Kenworthy, D. Apai, E. Mamajek, & M. Meyer Thermal IR enables the study of mature stars, which are common and thus nearby, providing fine physical resolution, and modest model uncertainties.

16. Direct (Non) Detections of Gas Giant Planets No massive planets at large orbital radii. [3 Mjup @ 30 AU] dN/da ~ a p Lafrenerie et al. (2007); Biller et al. (2007); Kasper et al. (2007); Apai et al. (2008); Heinze et al. (in prep)

18. Benefits of Direct Detection :  Enable estimate of internal energy source of planet: » Assess energy available for life. » Viability of planet tectonics? [Valencia et al. 2007].  Enable study of atmospheric composition: » Assess possible surface chemistry. » Non-equilibrium chemistry [Kaltenegger et al. 2007]?  Unique tool to understand planet formation! »‘Merger tree’ determines heating (volume) to cooling (surface area).

19. Observational Constraints on Planet Formation: Detecting Hot Protoplanet Collision Afterglows? Mamajek & Meyer (2007); Miller-Ricci et al. (submitted)

20. Putting it All Together: Surveyed To date.

21. Putting it All Together: Surveys underway.

22. Putting it All Together: GMT Survey.

23. Putting it All Together: If terrestrial Planets are Common GMT Discovery Space…

24. Solar System Exploration on the Cheap! Water on Enceladus detected by Cassini Searching for Methane on Mars

25. My ELT: Required Capabilities  Aperture > 20 meter (resolution over light-gathering)! » Piecing the “confusion-limited” veil…  Diffraction-limited imaging from 1-25 microns. » To reach < 3 AU around nearest young stars.  Near-/Mid-IR spectral resolution: R=30,000/50,000. » Origins of the cold and slow…  Near-/Mid-IR Field of View: > 2 arcminutes. » Size of nearest rich star clusters.  Precision visible RV: R = 40,000. » Earth-mass planets around late-type stars.

26. Take Home Message: The GSMT…..  Will play a key role in understanding star formation, planet formation, and the pathways enabling chemistry of life.  Is extremely complementary to JWST and ALMA.  Will help frame science questions for next generation missions with astrobio relevance (space strategic mission concepts as well as flagship missions).  Technology development on ground-based facilities can enhance flight programs.  Can be a concept for the COMMUNITY to participate in the LBT, the TMT, the GMT, and more!

27. Observational Constraints on Planet Formation: Detecting Hot Protoplanet Collision Afterglows? Mamajek & Meyer (2007); Miller-Ricci et al. (submitted)