Download 8 m Club Meeting - Adaptive optics

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
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 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)
4
WMKO Chronology (cont.)
•
•
•
•
•
•
•
•
•
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
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
NIRC2
NIRSPEC
or Dual Star
Module
Nasmyth
Platform
Rails to deck
Electronics
Racks
11
12
Wavefront Sensor Path
Field Steering Mirrors (2 gimbals)
Sodium dichroic/beamsplitter
AOA Camera
Video Display
AOA Camera
Camera Focus
Wavefront Sensor Focus
13
Wavefront Sensor Optics: field stop, pupil relay, lenslet, reducer optics
14
Science Instruments
Science Instruments
•
K1&2:
– Interferometer (AO): Visibility, Nulling, Differential Phase
•
K1:
– HIRES
– LRIS
– LWS
– NIRC
•
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/
15
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
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
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
•
21
High-resolution imaging of disks in which planets may be forming
Keck Basement
22
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