Transcript 8 m Club Meeting - Adaptive optics

Keck Observatory
Overview
Peter Wizinowich
W. M. Keck Observatory
AOSC
May 31, 2004
Presentation Sequence
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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.)
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1991 1992 1993 1996 1996 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) 1st light
Keck-Keck first fringes
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
Enclosure with
roof removed
Elevation
Ring
AO Optics
Bench
NIRC2
NIRSPEC
or Dual Star
Module
Nasmyth
Platform
Rails to deck
Electronics
Racks
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Wavefront Sensor Path
Field Steering Mirrors (2 gimbals)
Sodium dichroic/beamsplitter
AOA Camera
Video Display
AOA Camera
Camera Focus
Wavefront Sensor Focus
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Wavefront Sensor Optics: field stop, pupil relay, lenslet, reducer optics
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Science Instruments
Science Instruments
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K1&2:
– Interferometer (AO): Visibility, Nulling, Differential Phase
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K1:
– HIRES
– LRIS
– LWS
– NIRC
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HIgh Resolution Echelle Spectrometer
Low Resolution Imaging Spectrometer
Long Wavelength Spectrometer
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!
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
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FWHM = 50 milli-arcsec
Galactic: Galactic Center (Ghez et al.)
K-band
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First LGS Results
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Keck Interferometer
Characteristics
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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
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High sensitivity fringe visibility measurements
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Measurement of zodiacal dust around nearby stars using nulling (TPF)
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Direct detection of brown dwarfs & warm Jupiters (Jupiter-mass
planets in close orbits)
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Indirect detection of Uranus-mass planets via astrometry
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High-resolution imaging of disks in which planets may be forming
Keck Basement
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OHANA: The Mauna Kea
Observatory
Subaru
8m
UKIRT
4m
Gemini
8m
CFHT
3,60 m
Keck I&II
10 m
IRTF
3 m -> 6,50m
• Largest optical astronomical site of quality in the world
• 3 4m-class telescopes and 4 8-10m-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 using single-mode fibers