TMT: A Progress Report

Mike Bolte, Ray Carlberg, Chuck Steidel, Steve Strom

Presented to the GSMT SWG12 February, 2004

Outline

• TMT Project Status Report– Caltech, UC, ACURA and AURA partnership– Outline of the Design and Development Phase

• The TMT Science Requirements Document– Representative science cases– Prioritized observatory capabilities

The TMT Partnership

• In June, 2003 AURA & ACURA signed Letters of Intent to partner with UC & Caltech to design a 30-m telescope– Private funding (~$35M) already committed to Design &

Development program• Will result in a costed Preliminary Design in Q4 2007

– Publicly funded (US + Canada) complement will enable: • Fast-track toward design: completion early in JWST era

• Public participation through AURA; ACURA in key design decisions

Goals of the TMT Partnership

• Combine the strengths of public and private observatories to create a 30-m telescope (TMT)– Contemporary with JWST/ALMA – Following the recommendation of the AASC decadal review:

• Involve the community in defining observatory goals• Public access to TMT in proportion to federal investment

• Maximize community benefit via federal investment in technology development common to all ELT programs– Sites– Durable coatings– AO components……etc.

Top-level ScheduleALMA Operations

D&D Phase

JWST Launch

Comparison of Point DesignsGSMT CELT VLOT

www.aura-nio.noao.edu/ http://celt.ucolick.org/ http://www.hia-iha.nrc-cnrc.gc.ca/VLOT/index.html

Comparison of Point Designs

Below primaryAbove primaryBelow primaryElevation axisVertical Nasmyth

(fixed gravity orientation)

NasmythPrime FocusCassegrain FocusFixed-gravity Cass.

Nasmyth (MCAO relay)

Instrument Locations

Alt-Az: large elevation journals

F/15Active3.96 m1080

45 mm1.0 m across corners

F/1.530 m

At primary mirror

Ritchey-ChrétienCELT

F/15F/18.75Final Focal RatioAlt-Az: large elevation

journalsAlt-Az: radio telescopeTelescope Structure

20 m30 mM1 DiameterF/1.0F/1.0M1 Focal Ratio

1.8 m across corners1.33 m across cornersSegment Size80 mm50 mmSegment Thickness

150618Number of Segments2.5 m2 mM2 DiameterActiveAdaptiveM2 Configuration

At primary mirrorAt secondary mirrorAperture Stop

Ritchey-ChrétienCassegrainOptical DesignVLOTGSMTDesign Feature

Goals of the D&D Phase

• Define the Science Requirements

• Establish observatory design that meets the requirements

• Define the schedule to build TMT

• Define the cost to build & operate TMT

• Define the cost to upgrade TMT during operations

• Select the site

Goals of the D&D Phase

• Develop an observatory operations plan

• Develop a risk mitigation plan

• Develop a proposal for TMT construction

• Unite the community behind TMT

Key Design Decisions• Primary mirror focal ratio• Segment configuration, size & thickness• Segment material• Adaptive vs active secondary• Gregorian vs Cassegrain secondary• Nasmyth only vs multiple foci• Location of elevation axis: above vs below primary• AO modes to be included;

– Division of AO between telescope and instruments

• Configuration of enclosure

Key Technology Investments

• Adaptive M2 approaches• Durable coatings• SiC segments• Site evaluation• Gratings (e.g., immersed Si; large mosaics; large VPH)• Instrument concepts• AO components

NB: Federally-funded studies will be competed openly

Time-Critical Interim Tasks

Systems EngineeringHIAGlen HerriotSystems Engineering InstrumentationCITKeith TaylorWFOS Design Study

UCTerry MastStressed-Mirror PolishingNOAOMyung ChoSilicon Carbide Segments

Adaptive OpticsCITRich DekanyAdaptive OpticsAdaptive OpticsNOAOBrent EllerbroekAdaptive Secondary Mirrors

HIAJim StilburnDurable CoatingsInt. ModelingHIAJennifer DunnIntegrated ModelingSite TestingCITMatthias SchoeckSite Testing

Associated WGAffil.Interim ManagerTask

Adaptive Optics Working Group

Rich Dekany CITMatthew Britton CITGlen Herriot HIAJean-Pierre Veran HIADon Gavel (Chair) UCSC-CfAOClair Max UCSC-CfAOBrent Ellerbroek AURA- NOAOFrancois Rigaut AURA- Gemini

Integrated Modeling Working Group

Joeleff Fitzsimmons HIAJennifer Dunn HIAGeorge Angeli (Chair) AURA-NIOKonstantinos Vogiatzi AURA-NIOAndy Sheinis UCSC-CfAOJim Brase UC-LLNLDoug MacMartin CITRich Dekany CIT

Instrumentation Working Group

Doug Simons AURA-GeminiDavid Sprayberry AURA-NOAOJames Larkin UCLASteve Vogt UCSCKeith Taylor CITKeith Matthews CITDave Crampton (Chair) ChairGordon Walker UBC

Sites Working Group

Derrick Salmon CFHTEric Steinbring HIAAlistair Walker (Co-chair) AURA-NOAODave DeYoung AURA-NOAOGeorge Djorgovski (Co-chair) CITMatthias Schoeck CITGary Chanan UCIJames Graham UCB

Systems Engineering Working Group

Glen Herriot HIA ChairToomas Erm CITEric Hansen AURA-NIOTerry Mast UCSC

Adaptive Optics Development

Eric JamesLaurent JolissantJean-Francois LavigneJeff LeDueBruce MacintoshKeith MatthewsClaire MaxDave PalmerHongwu RenFrancois Rigaut

Aron AhmadiaBrian BaumanMatthew BrittonRichard DekanyBrent EllerbroekMurray FletcherDon GavelJames GrahamEric HansenGlen Herriot

Anna SergussonAndrew Sheinis Eric SteinbringJeff StoeszMitchell TroyRobert UptonViswa VelurJean-Pierre Veran

Adaptive Secondary Mirror

Participants:George Angeli Richard DekanyBrent EllerbroekDon Gavel Eric HansenTerry MastJerry NelsonRichard Robles Larry SteppRobert UptonJean-Pierre Veran

Durable High-Performance Coatings

Participants:Maxime Boccas Bill BrownEric HansenDrew Phillips Jim Stilburn

Integrated Modeling

Participants:George Angeli Jim BraseKevin Cooper Rich Dekany Jennifer DunnBrent Ellerbroek Toomas Erm Joeleff Fitzsimmons Brooke GregoryGlen HerriotDoug MacMartin

Mahmoud Mamou Tait Pottebaum Scott RobertsAnna SegursonAndy Sheinis Anna Stuckas Robert UptonKonstantinos VogiatzisRaymond YuChris White

Silicon Carbide Segments

Participants:Myung ChoEric HansenTerry MastEarl Pearson Kei SzetoRobert Upton

Stressed-mirror polishing

Participants:Barry AlcottJerry CabakMyung ChoDeborah CulmerWill DeichEric HansenDavid HilyardLee Laitermann

Jeff LewisTerry MastJerry NelsonLarry SteppDean Tucker

Systems engineering

Participants:Gary Chanan Toomas ErmEric HansenGlen HerriotTerry MastJerry Nelson Scott Roberts Les SaddlemyerLarry SteppKeith Taylor

Wide-Field Optical Spectrograph Design Study

Participants:Sebastien Blais-Ouellette David Crampton Harland Epps Denis Laurin Joe MillerBev Oke Ian Powell Kei Szeto Keith Taylor

TMT Science Requirements Document

• Responsibility of the TMT SAC

• Starts from CELT, GSMT and VLOT science cases

• Identifies capabilities needed for high impact science

• Prioritizes capabilities

SRD: Key Science Themes

• Exploration of galaxies and large-scale structure in the young universe

• Exploration of the ‘dark ages’ when the first sources of light were forming

• Exploration of the star- and planet- formation process

• Characterization of exo-planets

Science with TMT

The physics of young Jupiter's

Science Enabled by TMT• Tomography of the Intergalactic Medium at z > 1.5

– High resolution spectra of IGM absorption spectra• Determine 3-dimensional distribution of gas• Track evolution of metal abundance & relate to galactic activity

• Observing the galaxy assembly process– Integral field unit spectra of pre-galactic fragments

• Determine gas and stellar kinematics; measure mass directly• Quantify star formation activity and chemical composition

• Separating constituent stellar populations in galaxies– MCAO imaging and spectroscopy

• Determine age and distribution of chemical abundances

• Understanding where and when planets form– Ultra-high resolution mid-IR spectra of ~1000 accreting PMS stars

• Infer planetary architectures via observation of ‘gaps’ in disks

• Detecting and characterizing mature planets– Extreme AO coronography; spectroscopy

Probing the Distant Universe

IGM Tomography

• Goals:– Map out large scale structure for z > 1.5– Link emerging distribution of gas; galaxies to CMB – Determine metal abundances

• Measurements:– Spectra of 105 QSOs and galaxies (R ~20000)

• Key requirements:– 10-20’ FOV; ~1000 slits

Probing Forming Galaxies• Goals:

– Determine gas and stellar kinematics– Quantify SFR and chemical composition

• Measurements:– Spectroscopy of H II complexes and underlying stars

• Key requirements:– Deployable IFUs feeding R ~ 10000 spectrograph– Field of view to sample multiple systems

– 20 mas resolution (150 pc at z ~ 3)

Connecting the Distant & Local Universe

Stellar Populations• Goals:

– Quantify ages; [Fe/H]; for stars in nearby galaxies spanning all types– Use ‘archaelogical record’ to understand the assembly process– Quantify IMF in different environments

• Measurements:– CMDs for selected areas in local group galaxies – Spectra of ~ 105 stars in rich, forming clusters (R ~ 1000)

• Key requirements:– MCAO delivering 2’ FOV; MCAO-fed NIR spectrograph

Deconstructing Nearby Galaxies

Stellar Populations in Galaxies20”

M 32 (Gemini/Hokupaa) TMT with MCAO JWST

Population: 10% 1 Gyr ([Fe/H]=0), 45% 5 Gyr ([Fe/H]=0), 45% 10 Gyr ([Fe/H]=-0.3)

Simulations from K. Olsen and F. Rigaut

Origins of Planetary Systems

• Goals:– Understand where and when planets form– Infer planetary architectures via observation of ‘gaps’

• Measurements:– Spectra of 103 accreting PMS stars (R~105; λ ∼ 5µ)

• Key requirements:– On axis, high Strehl AO; relatively low emissivity– Exploit near-diffraction-limited mid-IR performance

Probing Planet Formation with High (105) Resolution Mid-Infrared Spectroscopy

Planet formation studies in the mid-IR (5-30µm)

Probe forming planets in inner disk regions

Residual gas in cleared region low τ emission

Rotation separates disk radii in velocity

High spectral resolution high spatial resolution

H2H2

Detecting and Characterizing Exo-Planets

• Goal: Image and characterize exo-planets – Mass, radius, albedo– Atmospheric structure– Chemistry– Rotation– “Weather”

• Measurements: R~ 10 photometry & R ~ 200 spectra– Near-infrared (reflected light)– Mid-infrared (thermal emission)

• Requirements:– Ex-AO capable of >0.9 Strehl– Coronagraphic imager– Smooth segments; closely-spaced segments; clean optics

Key Parameters: 30m TMT

1.6 AU

0.4 AU

Separation @ 10pc

160 mas4.7 µ

40 mas1.2 µ

5 λ/Dλ

Aperture is critical to enable separation of planet from stellar image

SRD: Required Capabilities

• Diffraction-limited imaging and spectroscopy in the 0.8-2.5 µm region over a 1-2’ FOV

• Seeing-limited spectroscopy (100 < R < 7000) in the 0.32-1.0 µm region over a 10-20’ FOV

• High resolution spectroscopy (20000 < R < 100,000) in the 1-5 µm and 7-28 µm range

SRD: First Light Instruments

• MCAO-fed deployable IFU spectrograph-imager

• Wide-field optical spectrograph

• Mid-IR Echelle spectrograph

• Near-IR Echelle spectrograph

SRD: Second Generation Instruments

• High resolution optical spectrograph• GLAO-fed near-IR MOS/IFU• MCAO-fed near-IR imager• Extreme AO coronagraph• Mid-IR imager/low resolution spectrograph

SRD: First Light AO Systems

• Low-order AO feeding mid-IR instruments– Adaptive M2?

– Separate cryogenic system?

• MCAO system:– MOAO (?) system for feeding IFUs

– Imager exploiting center of MCAO field

– On-axis feed for near-IR Echelle

SRD: Possible Gen II AO Systems

• Ex-AO system– Advance to Gen I if technology permits

• GLAO feeding deployable IFU spectrographs