Keck Observatory Overview Peter Wizinowich W M Keck

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

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

The People • 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 3

WMKO: A Brief Chronology • Early 1980 s – University of California and Caltech begin discussions to build “TMT” • 1985 - W. M. Keck Foundation provides $70 M 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 $63 M) 4

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

Mauna Kea Summit 6

Keck Telescopes 7

Primary Mirror 8

Primary Mirror Segments 9

Keck Telescope 10

Nasmyth Platform Enclosure with roof removed Elevation Ring AO Optics Bench NIRC 2 NIRSPEC or Dual Star Module Nasmyth Platform Rails to deck Electronics Racks 11

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

14 Science Instruments

Science Instruments • K 1&2: – Interferometer (AO): Visibility, Nulling, Differential Phase • K 1: – HIRES – LRIS – LWS – NIRC • HIgh Resolution Echelle Spectrometer Low Resolution Imaging Spectrometer Long Wavelength Spectrometer Near Infra. Red Camera K 2: – DEIMOS DEep Imaging Multi-Object Spectrograph – ESI Echellette Spectrograph and Imager – NIRC 2 (AO) Near Infra. Red Camera – NIRSPEC (/AO)Near Infra. Red Spectrometer – OSIRIS OH Suppression Infra. Red Integral field Spectrometer http: //www 2. keck. hawaii. edu/inst/ 15

D = 10 m! 16

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L dwarf companion to HR 7672 (Liu et al, Ap. J 571, 2002) NIRSPEC K-band image & spectra Closest ultracool companion around a main sequence star m = 8. 6 mag 18 FWHM = 50 milli-arcsec

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

First LGS Results 20

Keck Interferometer Characteristics • The two 10 -m Keck telescopes + 4 • • • Objectives 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 • 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 • 21 High-resolution imaging of disks in which planets may be forming

Keck Basement 22

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