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 InstrumentsInstrumentation 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 m; 5m 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 m; 5m goal)

• MIRES - R ~ 105 spectrograph (5-30 m)

• WFOS - kiloslit wide-field optical spectrograph

Lenslet Optics AO Focus

ReimagingCollimators

Filters

ReimagingCameras

Fold Mirror& Lenslet Array

SpectrographCollimator Mirrors (TMA)

Grating

Fold Mirror

SpectrographCamera Mirrors (TMA)

Detector

IRIS:UCLA ledcollaboration

ImageSlicer

FiberBundle

LensletArray

Focal Plane Feed to Spectrograph Detector

1 2 3 4

Deconstructing Forming Galaxies at 7 mas resolution

MIRES (UH; NOAO; UCD; Texas)

Echelon is ~1 m long

Planet Formation Environments

0.1 AU~1000 K

1 AU~200 K

10 AU~50 K

H2O ro-vib

CO v=2

CO v=1

H2 UV, NIR, MIR

OH v=1

Study gas dissipation timescale: constrains pathways for giant planet formation, terrestrial planet architectures

Studying gas in disks:

(thermal)

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

• 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.

HROS spectra of metal-poor stars

U Colorado HROS Concept

PFI Science Missions

Science role Star H magnitude

Distance 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:

– 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

• Design M2 and M3 support and control system• Design Laser launch facility• Manage site evaluation process• Develop observatory requirements document• Provide engineering support: CFD; opto-

mechanical design• Design MIRES (UH-NOAO collaboration)