Transcript Keck Observatory in the TMT Era

Keck Observatory in the TMT
Era
Keck Strategic Planning meeting
September 18, 2009
TMT has selected 13N at
Mauna Kea
• MK process
• CMP subplans need to be
completed
• Final EIS submitted and
accepted
• CDUA application prepared
and submitted
• CDUP issued
• Legal issues resolved
• Schedule, with legal
challenge periods included
and optimistically assuming
success has CDUP issued in
October 2010
TMT Early-Light capabilities
• MOBI: 0.32µ - 1µ, R=1000, 3000, 8000 (0.7
slit width), 40 arcmin2
LRIS-like with added
cross-dispersed higher-R
mode
NFIRAOS
• TMT AO system is designed to deliver
rms wavefront error of 190nm and to
pass a 2-arcminute (diameter) field, with
good correction over 30-arcsecond
(diameter) field.
• Performance is comparable to NGAO
TMT First Decade Instrument/Capability Suite
Instrument
Near-IR DL Spectrometer &
Imager
(IRIS)
Spectral
Resolution
~4000
Wide-field Optical
Spectrometer
(WFOS)
1000-5000
Multi-slit near-DL near-IR
Spectrometer
(IRMS)
2000 - 5000
Mid-IR Echelle
Spectrometer & Imager
(MIRES)
5000 - 100000
ExAO I
(PFI)
50 - 300
High Resolution Optical
Spectrograph
(HROS)
30000 - 50000
MCAO imager
(WIRC)
5 - 100
Near-IR, DL Echelle
(NIRES)
5000 - 30000
Science Case
Assembly of galaxies at large redshift
Black holes/AGN/Galactic Center
Resolved stellar populations in crowded fields
Astrometry
IGM structure and composition 2<z<6
High-quality spectra of z>1.5 galaxies suitable for measuring stellar
pops, chemistry, energetics
Near-field cosmology
Near-IR spectroscopic diagnostics of the faintest objects
JWST follow-up
Physical structure and kinematics of protostellar envelopes
Physical diagnostics of circumstellar/protoplanetary disks: where and
when planets form during the accretion phase
Direct detection and spectroscopic characterization of extra-solar
planets
Stellar abundance studies throughout the Local Group
ISM abundances/kinematics, IGM characterization to z~6
Extra-solar planets!
Precision astrometry
Stellar populations to 10Mpc
Precision radial velocities of M-stars and detection of low-mass
planets
IGM characterizations for z>5.5
5
IRIS - Infrared imaging spectrometer
IRIS is OSIRIS-like. Works at
diffraction limit, multiple plate
scales
imager filter
wheels
2’
IRIS dewar
(at 77k)
WFS
IFUs
Grating
imager
F/15 AO Focus
Common
spectrograph
and camera
for both IFUs
IRMS - Infrared multislit spectrometer
0.8 - 2.5 um cryogenic
multi-slit spectrometer
2.3 arcmin field of view
0.06 arcsec sampling
46 moveable slits 2.4” long
Covers entire Y, J, H or K
band at R = 4660
TMT Schedule
• Current first-light date with NFIRAOS, MOBIE,
IRMS and IRIS is Fall 2018
• This is based on a resourced schedule and
some assumptions about completing the
partnership and feeding funding to the project.
• Not likely to be delivered any earlier than this
• Commissioning will be carried out over irst two
years (only part of the time will be available for
science)
Keck in the TMT Era
• Complementary capabilities
–
–
–
–
Wider-field MOS
High-R at all wavelengths
Visible-light AO
Natural complementarity set by source brightness
• Feeder capabilities
• Complementary uses
– Concentrate on larger programs
– Concentrate on specialized instruments