Transcript Studying gas in disks

Characterizing Exoplanets: The Challenge
GSMT Potential
• GSMT will detect & classify Jovian mass planets, from ‘roasters’
to ‘old, cold’ Jupiters located at ~ 5AU for stars at d < 10 pc
• Via photometry (R ~10) and low resolution spectroscopy (R ~200)
• Requires star suppression ~ 107
• Detection of lower mass planets is possible, but star suppression
must exceed 108
– Characterization via spectroscopy not possible
• GSMT will detect ‘warm Jupiters’ around t < 10 Myr stars in
nearby star-forming regions (75-150 pc)
ELT Projects
ESO OWL 100-m Concept
• 100m segmented primary
• Spherical segments
• NGS AO
• Find exo-earths
• Stellar populations to Virgo
• Design studies underway
• Major funding after ALMA
Magellan 20 Concept
• 7x8.4m primary at f/0.7
• Possible upgrade path to 20/20
• General purpose telescope
• wide FOV feeding MOS
• NGS AO
• MCAO
• ExAO planet finder
• Complete by 2014
• Partners: Carnegie, Arizona,
CfA, MIT, Michigan, Texas,
Texas A & M
20-20 Concept
• 7x8.4m primary at f/0.7
• 100-m baseline
• Detection of exo-earths
• Other high contrast scenes
• Magellan 20 + other partners?
TMT Reference Design
• 30-m segmented primary
• f/1 Gregorian
• 10’FOV, kilo-slit MOS
• Deployable IFUs + imager
• diffraction-limited
• 0.05” pixel
• R ~ 105 MIR spectrograph
• ExAO coronagraph
TMT Status
• Partnership formed
• UC, Caltech, Canada, AURA
• Reference design selected (Oct, 2004)
• based on CELT, VLOT and NIO/GSMT concepts
• Design and Development phase underway
• $70M effort
• Private funding committed (Moore Foundation)
• Public funding authorized (Canada; CFI)
• NSF funding (1/2 x $1M FY05; $2M FY06; ramp up in FY07)
• Site evaluation underway
• Conceptual Design Review: Spring, 2006
• Cost review: Fall, 2006
TMT First Light Instruments
Instrumentation priorities; requirements set by TMT SAC
– Includes one representative from the community; 2 planned
• NFIRAOS - facility AO system delivering narrow-field AO images
(1-2.5 mm; 5mm goal)
– 7 LGS constellation; deliver Strehl 0.7 images at K over 10”
• Upgrade to 30” FOV by adding DMs
– Feeds IRIS; NIRES; WIRC (see below)
• IRIS - IFU spectrograph/imager (1-2.5 mm; 5mm goal)
• MIRES - R ~ 105 spectrograph (5-30 mm)
• WFOS - kiloslit wide-field optical spectrograph
IRIS:
Fold Mirror
& Lenslet Array
UCLA led
collaboration
Lenslet Optics
Filters
Reimaging
Cameras
Grating
Spectrograph
Collimator Mirrors (TMA)
Detector
Fold Mirror
Spectrograph
Camera Mirrors (TMA)
AO Focus
Reimaging
Collimators
Deconstructing Forming Galaxies
at 7 mas resolution
Focal Plane
1
Image
Slicer
Fiber
Bundle
Lenslet
Array
2
3
4
Feed to Spectrograph
Detector
MIRES (UH; NOAO; UCD; Texas)
Echelon is ~1 m long
Planet Formation Environments
Studying gas in disks:
H2 UV, NIR, MIR
H2O ro-vib
OH Dv=1
CO Dv=1 (thermal)
CO Dv=2
0.1 AU
~1000 K
1 AU
~200 K
Study gas dissipation timescale: constrains pathways for
giant planet formation, terrestrial planet architectures
10 AU
~50 K
TMT Gen II Instruments
• HROS - R ~70,000 optical spectrograph
• IRMOS - deployable IFU IR spectrograph
• WIRC - wide-field IR camera (MCAO)
• NIRES - near-IR Echelle (R ~ 70,000)
• PFI - ExAO imager (106 - 107 contrast)
Metal-poor Stars with HROS
HROS spectra of
metal-poor stars
• The nucleosynthetic “fingerprints” of
Pop III stars, and the rare-earth
elements produced in SN explosions
are best observed at visible
wavelengths.
• R>30,000 required for reliable
measurements of abundances even for
very metal-poor stars.
• Need TMT to be able to push out to
other galaxies in the Local Group.
U Colorado HROS Concept
PFI Science Missions
Science role
Star H
Distance
magnitude
Angular
separation
Contrast
Very young planetary
systems (1-10 Myr)
8-11
50-150 pc
0.04-0.1”
(5 AU)
10-6
Planetary census
5-7
10-30 pc
>0.05” (1 AU
@ 20 pc)
10-8
Planetary R=1000
spectroscopy
5-8
10-50 pc
>0.1”
10-7
Circumstellar debris and
zodiacal dust
5-8
10-50 pc
>0.05” (0.5
AU@10 pc)
polarimetry
TMT Operations Model
• Plan for queue and classical operation
• Invest in end-to-end system that envisions
– Data reduction by PI and teams
– Extensive post-proprietary period mining of archives populated by well
characterized data
• Community participation via
– Classical or queue PI-mode observing
– Planning and executing Legacy surveys
• Community input needed
– Desired operations modes
– Mechanism for carrying out precursor/planning observations
Site Evaluation
GSMT Site Evaluation
• NIO is involved in testing multiple sites:
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–
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Las Campanas
Three Chilean Sites
Mauna Kea ELT site
San Pedro Martir
• Status:
– Remote sensing studies (cloud cover; water vapor) nearly complete
• MK / US / Chile comparison to finish in August
– CFD modeling of sites: good progress on first three sites
– Weather stations deployed on several mountains
– Multi-Aperture Scintillation Sensor (MASS)
• Measure turbulence profile above site
• In combination with DIMM, quantify contribution of ground-layer
Remote Sensing Survey
of Cloud Cover and PWV
• Survey uses meteorological satellite images
• Long time baseline
• Well-defined methodology provides:
– Photometric, spectroscopic, unsuitable conditions
based on cloud cover
– Precipitable water vapor above the sites
• Dispassionate comparison thus possible
• Areas studied:
– Northern Chile
– SW USA-Mexico
– Mauna Kea – Chile comparison
Computational Fluid Dynamics
• Characterize wind flow allowed pre-selection of sites
– Wind intensity
– Turbulence characteristics
– Down-wind wakes
• Characterization of all candidate sites now completed
Weather Station
Combining MASS + DIMM Results
Free atmosphere seeing steady at ~ 0.25” for 4 nights
Advancing US ELT Efforts
Advancing US ELT Efforts
• AURA goals:
– Ensure availability of ELT(s) early in the JWST era
– Ensure broad community access
– Provide a community voice in shaping ELT designs
AURA’s Approach
• Goal:
– Advance the design of TMT and GMT so that performance,
cost, schedule and risk of differing approaches can be assessed
• Provide $17.5M for TMT partnership
– NSF dollars leveraged 3:1
• Provide comparable funds for GMT
– Include funds for instrument concepts; technology
– Program will be open to the entire US community
Investment in TMT
• Responds directly to AASC recommendations
• The community will receive observing time in proportion
to the public investment
• AURA is represented at all levels in the project
– The community has a ‘seat at the table’ throughout the Design
and Development Phase
• TMT Partners committed to engaging the community
– Involve US and Canadian communities in instrument design
– Involve US community members in the TMT SAC
Advantages of AURA’s Approach
• Directly responsive to SWG recommendations
– Will fund two ELT programs: GMT and TMT
• US community is engaged in ELT efforts and will receive time in
proportion to federal investment in all ELTs
• Open dialog between projects benefits all and leaves open a
‘convergence path’
• Technology investment in ELT programs will result in significant
gains for existing telescopes
Initial NSF funds received ($1M for FY05; $3M in FY06)
Ramp up in FY 07
NIO Roles
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Design M2 and M3 support and control system
Design Laser launch facility
Manage site evaluation process
Develop observatory requirements document
Provide engineering support: CFD; optomechanical design
• Design MIRES (UH-NOAO collaboration)