Keck ObservatoryOverview

Peter WizinowichW. M. Keck Observatory

AOSCMay 31, 2004

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Presentation Sequence

• Brief Chronology

• Telescopes & Optics

• Science Instruments

• Science at Keck

• Adaptive Optics

• Interferometer

• The People

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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

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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)

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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) 1st light • 2001 - Keck-Keck first fringes• 2003 - Keck II Laser Guide Star AO 1st light

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Mauna Kea Summit

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Keck Telescopes

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Primary Mirror

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Primary Mirror Segments

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Keck Telescope

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Nasmyth Platform

NIRC2

NIRSPECor Dual StarModule

ElevationRing

Enclosure withroof removed

ElectronicsRacks

AO Optics Bench

Rails to deck

NasmythPlatform

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Wavefront Sensor Path

AOA Camera

AOA CameraVideo Display

Sodium dichroic/beamsplitterField Steering Mirrors (2 gimbals)

Camera Focus

Wavefront Sensor Focus

Wavefront Sensor Optics: field stop, pupil relay, lenslet, reducer optics

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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/

D = 10m!

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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 magFWHM = 50 milli-arcsec

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Galactic: Galactic Center (Ghez et al.)

K-band

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First LGS Results

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Keck InterferometerCharacteristics• 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

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Keck Basement

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CFHT3,60 m

Gemini8 m

UKIRT4 m

Subaru8 m Keck I&II

10 m

IRTF3 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