Giant Magellan Telescope Project Science Drivers & AO Requirements

1. Giant Magellan Telescope Project Science Drivers & AO Requirements Patrick McCarthy - GMT Director Phil Hinz & Michael Hart - GMT AO Team AO4ELT - Paris 2009 AO4ELT - June 22, 2009

2. The GMT Partners • US Institutions • Carnegie Institution • Harvard University • Smithsonian Institution • Texas A&M University • University of Arizona • University of Texas Austin • International Institutions • Astronomy Australia Limited • Australian National University • Korea Astronomy & • Space Science Institute AO4ELT - Paris 2009

3. The GMT Concept Giant-Segmented Mirror Telescope 10mas @ 1μm 380 sq. meters f/8 Gregorian Segmented Adaptive Secondary Natural Seeing 20 FOV Ground-Layer Correction 8 FOV Diffraction-limited 20- 40 FOV AO4ELT - Paris 2009

4. Gregorian Instrument Mounting Survey, GLAO, & Mid-IR instruments below LTAO instruments above AO4ELT - Paris 2009

5. Instrument Platform Top Layout AO relay Natural seeing instruments GLAO/LGS wavefront sensors 16 m AO instruments 10 m AO4ELT - Paris 2009

6. Gregorian Instrument Rotator Instrument platform (IP) Multiple instrument mounting GLAO & Mid-IR Instruments AO4ELT - Paris 2009

7. Instrument Development NIRMOS GMTNIRS GMACS Mode: AO = adaptive optics, NS = natural seeing AO4ELT - Paris 2009

8. AO Science Drivers Exoplanet Studies Imaging exoplanets in reflected light Thermal radiation from young exoplanets Structure of debris disks Stellar Populations IMF variations Star Formation Histories Black Hole Demographics Galaxy Assembly Structure & Dynamics of Galaxies at z > 2 First Light Studies AO4ELT - Paris 2009

9. Detect 5-10 MJ giant planets 100-300 zody warm debris disks Detect <1 MJ planets 3-10 zody warm debris disks L band detection limit 16x improved with ~4x larger diameter Mid-IR Imaging of Exoplanets • 3.8 um: 25 Jy 10 um: 750 Jy • 3 λ/D: 0.48” 3 λ/D: 1.0” • 3.8 um: 1.5 Jy 10 um: 45 Jy • 3 λ/D: 0.11” 3 λ/D: 0.25” 1 hour 5 sigma limits HR8799 MMT GMT can undertake comprehensive study of giant planets in > 3 AU range around stars at 30 pc. AO4ELT - Paris 2009

10. Nascent Planetary Systems • Pic at 11m • Gemini JWST JWST GMT 10 AU GMT ALMA ELTs have the spatial resolution to probe the zone where Earth-like rocky planets live AO4ELT - Paris 2009

11. Resolving Distant Stellar Systems with AO Globular Cluster around Cen A 3.8Mpc 3pc core radius H-band HST Gemini GMT 4mas pixels 2 Laser Tomography Adaptive Optics AO4ELT - Paris 2009

12. Resolving Distant Stellar Systems with AO Globular Cluster around Cen A 3.8Mpc 3pc core radius H-band Gemini 8m GMT 25m AO4ELT - Paris 2009 12

13. UDF 6462, H-band, NIFS, Hα z = 1.57, MB = -21.0, 5 hr object, 5 hr sky HUDF - i NIFS - Sum Clump cluster AO4ELT - Paris 2009

14. UDF 6462, H-band, GMTIFS, Hα z = 1.57, MB = -21.0, 5 hr object, 5 hr sky HUDF - i GMT - Sum Clump cluster AO4ELT - Paris 2009

15. Image Sharpening with GLAO GLAO Native Seeing 15 x 15 60 mas pixels 0.5 FWHM 0.15 FWHM The GMT architecture is ideally suited for Ground-Layer AO AO4ELT - Paris 2009 15

16. Adaptive Optics Prioritization Three guiding considerations: 1. The AO system should allow us to meet our science goals 2. It should build on the natural strengths of the GMT - low thermal IR foot print - ground-layer conjugation with wide-field of view - clean diffraction pattern 3. A clear upgrade path that uses much of the first generation hardware AO4ELT - Paris 2009

17. AO Science Targets Targets Requirements Exoplanets, debris disks, Diffraction-limited images & IFU Spectra AGN, black holes small sizes, low sky density, no multiplexing High Strehl, small field, low-background - Laser Tomography (LTAO) & NGS AO z > 2 galaxies Range of sampling scales, IFU & slit spectra small sizes, moderate sky density All-sky, range of Strehl, range of field, near-IR only - GLAO & LTAO Resolved stellar populations Diffraction-limited, emphasis on photometry range of sizes, low sky density All-sky, high Strehl, large field - LTAO &MCAO AO4ELT - Paris 2009

18. First Generation GMT AO Modes AO4ELT - Paris 2009

19. AO Features Unique to the GMT • ASM allows low background observations at > 2 µm. • For 25 m telescope, AO correction is needed even at 10 microns. • Exoplanet imaging and planet formation science drivers are strengthened by this design choice. • ASM and wide-field telescope design enables GLAO. • Will increase the sensitivity and resolution of the planned multi-object NIR and visible spectrographs for GMT. • Galaxy assembly and high-z science drivers are strengthened by this design choice.

20. System Performance • System is designed to maximize science return with minimal technical development: • Adaptive Secondary Mirrors are near-replicas of LBT, VLT design • Laser Guide Star system builds on Na laser development for current telescopes. • Laser Projection system is similar to MMT design. • Expected AO performance is similar to MMT/LBT systems. • Within the technical constraints above, the system performance and design is derived from the science requirements and the science instrument needs. GCAR, Pasadena CA, April 27-29, 2009 -- AO system

21. AO System Performance

22. AO System Performance NGS performance versus guide star brightness AO System Performance versus wavelength SM = 94% SL’ = 90% SK = 72% 2 ms 1 ms Strehl Ratio K band Strehl Ratio SH = 56% 5 ms SJ = 36% 10 ms Wavelength (µm) V magnitude (K5 star)

23. AO4ELT - Paris 2009

24. GMT 8.4m Off-Axis Prototype The first GMT primary segment is in the polishing/figuring stage Completion date: March 2010 GMT Segment #1 at the Steward Observatory Mirror Lab AO4ELT - Paris 2009

25. Schedule AO4ELT - Paris 2009

26. GMT’s AO Top-Level Requirements Play to its Strengths: Mid-IR with Adaptive Secondary Wide-field Ground-Layer AO Laser Tomography Seeing-Limited Requirements and Instruments are also important… High Dispersion Spectrographs Wide-field Multi-Object Spectrographs Astronomical Society of Australia Meeting - Perth July 08

27. Backup Slides

28. Adaptive Optics Prioritization GMT First Generation AO Modes: - “all sky” laser tomography AO high Strehl, 20 - 40 field of view, depending on  - Ground layer adaptive optics 8 diameter field, factor of 2 - 4 improvement in FWHM, EE - Natural guide star AO high Strehl, small field of view, low thermal IR background Upgrade modes: MCAO (2nd DM in AO relay) ExAO (2nd DM in instrument) AO4ELT - Paris 2009

29. Detect 5-10 MJ giant planets 100-300 zody warm debris disks Detect <1 MJ planets 3-10 zody warm debris disks L band detection limit 40x improved with ~3x larger diameter Mid-IR Imaging of Exoplanets 3.8 um: 25 Jy 10 um: 750 Jy 3 λ/D: 0.48” 3 λ/D: 1.0” 3.8 um: 0.6 Jy 10 um: 18 Jy 3 λ/D: 0.11” 3 λ/D: 0.25” 1 hour 5 sigma limits GMT can undertake comprehensive study of giant planets in > 3 AU range around stars at 30 pc. AO4ELT - Paris 2009

30. AO Imaging of Young Planets 2/D at 1.5m 42m 30m 25m 8m 8m Angular Separation (mas) AO4ELT - Paris 2009 30

31. top view AO System Layout LGS Projector Adaptive secondary mirror (ASM) Laser beam relay • AO Focal Plane Assembly (FPA) • Optical relay • LGS wavefront sensors • Phasing camera • AO instruments Laser house AO4ELT - Paris 2009

32. top view AO System Overview Laser Projector Adaptive Secondary Mirror (~4700 actuators) AO relay and Narrow-field WFS GLAO WFS Laser Housing AO4ELT - Paris 2009

33. Three independent measurements Principal optical test Full-aperture, interferometric test Scanning pentaprism test Measures low-order aberrations via slopes Laser Tracker Plus Scans surface with laser tracker Works on ground or polished surface AO4ELT - Paris 2009

34. Phase Apodization 1.65 m, 5% band. Diffraction only, no wavefront error 10-6 suppression at 4 /D, 56 mas 10-5 companion AO4ELT - Paris 2009

35. AO Imaging of Massive Planets 3/D at 1m Log Contrast 42m 30m 25m 8m Angular Separation (mas) AO4ELT - Paris 2009 35

36. AO Studies of Black Hole Demographics 1.22/D @1.5m 8m GMT AO4ELT - Paris 2009 36

37. AO Imaging of Young Planets 2/D at 5m GMT 8m 8m Angular Separation (mas) AO4ELT - Paris 2009 37