peter wizinowich w. m. keck observatory aosc may 31, 2004
DESCRIPTION
Keck Observatory Overview. Peter Wizinowich W. M. Keck Observatory AOSC May 31, 2004. Presentation Sequence. Brief Chronology Telescopes & Optics Science Instruments Science at Keck Adaptive Optics Interferometer The People. The People. - PowerPoint PPT PresentationTRANSCRIPT
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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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Scie
nce I
nstr
um
en
ts
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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/
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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