1. Keck Observatory Overview Peter Wizinowich W. M. Keck Observatory AOSC May 31, 2004

2. 2 Presentation Sequence Brief Chronology Telescopes & Optics Science Instruments Science at Keck Adaptive Optics Interferometer The People

3. 3 Science Community (Caltech, UC, NASA, UH, NOAO) –Astronomers (~ 300 users) –Graduate Students –Instrument Builders CARA (~120 staff) –Support Astronomers –Observing Assistants –Engineers & Techicians (Electronics, Facilities, Mechanical, Optical, Software) –Administrative Support (Human Resources, Financial, Administrative Assistants, Janitors, Maintenance) –Public Outreach

4. 4 WMKO: A Brief Chronology Early 1980s – University of California and Caltech begin discussions to build “TMT” 1985 - W.M. Keck Foundation provides $70M grant for Keck I –CARA established as a non-profit organization to build & operate the Keck telescopes. 1990 - Keck Foundation provides grant for 80% of Keck II actual construction cost (that grant eventually totals $63M)

5. 5 WMKO Chronology (cont.) 1991 - 5-m Keck I first light 1992 - 10-m Keck I first light 1993 - Keck I science operations begin 1996 -Keck II first light 1996 -Keck II science operations begin 1996 -NASA joins Keck partnership 1999 - Keck II Adaptive Optics (AO) 1 st light 2001 - Keck-Keck first fringes 2003 -Keck II Laser Guide Star AO 1 st light

6. 6 Mauna Kea Summit

7. 7 Keck Telescopes

8. 8 Primary Mirror

9. 9 Primary Mirror Segments

10. 10 Keck Telescope

11. 11 Nasmyth Platform NIRC2 NIRSPEC or Dual Star Module Elevation Ring Enclosure with roof removed Electronics Racks AO Optics Bench Rails to deck Nasmyth Platform

12. 12

13. 13 Wavefront Sensor Path AOA Camera Video Display Sodium dichroic/beamsplitterField Steering Mirrors (2 gimbals) Camera Focus Wavefront Sensor Focus Wavefront Sensor Optics: field stop, pupil relay, lenslet, reducer optics

14. 14 Science Instruments

15. 15 Science Instruments K1&2: –Interferometer (AO): Visibility, Nulling, Differential Phase K1: –HIRES HIgh Resolution Echelle Spectrometer –LRIS Low Resolution Imaging Spectrometer –LWS Long Wavelength Spectrometer –NIRC Near InfraRed Camera K2: –DEIMOS DEep Imaging Multi-Object Spectrograph –ESI Echellette Spectrograph and Imager –NIRC2 (AO) Near InfraRed Camera –NIRSPEC (/AO)Near InfraRed Spectrometer –OSIRIS OH Suppression InfraRed Integral field Spectrometer http://www2.keck.hawaii.edu/inst/

16. D = 10m!

18. 18 L dwarf companion to HR7672 (Liu et al, ApJ 571, 2002) NIRSPEC K-band image & spectra Closest ultracool companion around a main sequence star  m = 8.6 mag FWHM = 50 milli-arcsec

19. 19 Galactic: Galactic Center (Ghez et al.) K-band

20. 20 First LGS Results

21. 21 Keck Interferometer Characteristics The two 10-m Keck telescopes + 4 proposed 1.8-m telescopes 85-meter K-K baseline Wavelength: 2  m & 10  m Imaging resolution: 5 mas at 2  m Astrometric accuracy: 30  as First light –Two-element: March 2001 Objectives High sensitivity fringe visibility measurements Measurement of zodiacal dust around nearby stars using nulling (TPF) Direct detection of brown dwarfs & warm Jupiters (Jupiter-mass planets in close orbits) Indirect detection of Uranus-mass planets via astrometry High-resolution imaging of disks in which planets may be forming

22. 22 Keck Basement

23. 23 CFHT 3,60 m Gemini 8 m UKIRT 4 m Subaru 8 m Keck I&II 10 m IRTF 3 m -> 6,50m Largest optical astronomical site of quality in the world Unique opportunity to build the most resolving and sensitive interferometer with no competitor for more than a decade if telescopes are combined using single-mode fibers 3 4m-class telescopes and 4 8-10m-class telescopes with adaptive optics OHANA: The Mauna Kea Observatory