TMT Overview

1
TMT Capabilities 2004 Projection Keck Strategic
Planning Meeting UCLA 18 Sept 2004 Mike Bolte,
Chuck Steidel
2
TMT Partnership

• TMT is a four-way partnership formed in 2003
• Association of Canadian Universities for Research
  in Astronomy (ACURA)
• Association of Universities for Research in
  Astronomy(AURA)
• California Institute of Technology(CIT)
• University of California (statewide) (UC)
• Web site http//tmt.ucolick.org/

Collaboration formerly known as CELT
3
Project Organization

• Project manager Gary Sanders, formerly manager
  of LIGO
• Project scientist Jerry Nelson
• TMT Board of Directors
• Chairman of Board Ed Stone
• 3 members from each partner
• meets quarterly
• Science Advisory Committee (sets science
  requirements)
• 3 members from each partner
• 1 observatory director from each partner
• Project scientist
• Project office
• Location Pasadena
• Significant satellite activities anticipated at
  each partner location

4
Schedule

• Design Development Phase Schedule
• Start 2004 Apr
• Science-driven Requirements Document 2004 Jun
• Baseline design (key features set) 2004 Oct
• Conceptual design review 2006 Apr
• Request for construction funds 2006 Sep
• Preliminary design review 2007 Oct
• Construction start 2008 Jan
• Construction Schedule
• First light, partial segments 2013 Jul
• First light, all segments 2014 Apr

5
Funding

• Design Development Phase (4 year period, 70M)
• UC/Caltech
• Moore funds secured (17.5M17.5M)
• ACURA (Canada)
• Funding from Canadian Foundation for Innovation
• Support anticipated from several Canadian sources
• AURA (US national community)
• GSMT proposal submitted to NSF requests funds for
  TMT
• AURA New Initiatives Office supporting TMT
  activities (site testing, etc) at gt1M/yr
• Construction ( 6 year period)
• Estimated cost, including contingency 500-900M

Note 45Mltlt900M
6
Design Basics

• Basic design decisions already made
• 30-m filled aperture
• Points to most of sky above 2.4 airmasses
• Field of view 10 arcmin (goal 20 arcmin)
• Wavelength range 0.31 to 30 µm
• Aplanatic two-mirror telescope (RC or Gregorian)
• Segmented primary ( 500-1000 segments)
• Alt-az configuration
• Two major modes Adaptive optics, no adaptive
  optics
• Expect about half of telescope time to each
  (initially)

7
Science-driven Requirements

• The Science Advisory Committee and Project
  Scientist are responsible for developing and
  articulating the science case for TMT and
  defining the capabilities that will allow that
  science to be done.
• Some capabilities are mission driven based on
  specific science program objectives
• Some are based on gains to be made over
  anticipated 2014 facilities (e.g. some programs
  have sensitivities gains that scale like D2, some
  D4)
• Some fall in the category of broad capabilities
  that will serve the community well for all the
  exciting problems we cant anticipate today.
  This is the Keck model - provide broad
  capabilities to a talented community of users
  with guaranteed access and excellent science will
  result.

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Adaptive Optics

• AO general objectives
• Full sky coverage
• Strehl 0.5 at 1µm (wavefront errors 130 nm)
• Diffraction limit 0.007 arcsec at 1µm (l/D)
• Low emissivity/background
• large field of view
• MOAO - correction done for specific directions
• Laser-based tomographic system for measuring the
  atmosphere
• Correction system is driven by measurements
  (open-loop)
• Small field ( 10 arcsec)
• Multiple objects over wide field ( 5 arcmin)
• Mid-IR AO system
• Wide field imaging ( 30 arcsec, photometry,
  astrometry) with MCAO
• Extreme AO for planet detection
• Ground Layer Adaptive Optics?

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Science Instrument Concepts

• Small field, diffraction-limited, near IR
  spectrometer (IFU)-imager
• Wide field, near-DL, multi-IFU near IR
  spectrometers
• Wide field, optical, imaging spectrometer
  (multi-slit) (WFOS)
• Mid-IR echelle, diffraction-limited
• Extreme AO planet imager
• Near IR echelle, diffraction-limited
• Optical echelle, seeing-limited (MTHR)
• Moderate field, near IR, diffraction-limited
  imager (MCAO imager)

MOAO-fed
1st Generation
2nd Generation
Note fiscal and technical realities not yet
folded in (!)
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Small field, diffraction-limited, near IR
spectrometer (IFU) - imager Description

• Behind MOAO system
• Wavelength range 0.8-2.5µm
• Field of view 2 arcsec, 10 arcsec imaging
• Image quality diffraction limited
• Spatial sampling Nyquist sampled (l/2D) over
  32x32
• 
  over 10x10 arcsec for imaging
• Spectral Resolution 4000 2-50 for imaging

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Small field, diffraction-limited, near IR
spectrometer (IFU) - imager Science

• Spectroscopy of high-surface-brightness regions
  in distant galaxies
• Kinematics composition local SFR
• Galactic nuclei
• AGN, black holes in external galaxies
• Precision radial velocities at the Galactic
  center
• Spectroscopy of stars in crowded fields
• Stellar populations
• Cluster IMF studies

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Wide field, optical imaging spectrometer
(multi-slit) Description

• Wavelength range 0.31-1µm
• Field of view 75 arcmin2 (goal 300 arcmin2)
• Image quality 0.2 arcsec over 0.1µm, incl ADC
• Spatial sampling 0.15 arcsec
• Spectral resolution R300-5000 for 0.75 arcsec
  slit
• Throughput 30 0.31-1µm simultaneously
• Total slit length 300 arcsec
• Note this is the wide field mode for TMT
  (diameter 10?)

13
Wide field, optical imaging spectrometer
(multi-slit) Science

• Survey of IGM structure and chemical composition
  at high redshift from analysis of large samples
  of high S/N spectra of background QSOs and
  galaxies
• Survey of galaxy redshifts aimed at establishing
  LSS for z gt 1.5
• High-quality spectra of galaxies enabling
  constraints on stellar populations, galactic wind
  physics, chemistry, energetics
• Survey of stellar populations in the Local Group
  galaxies kinematics and composition
• Support of discoveries made using other
  facilities/techniques for redshift and other
  physical information

14
Multi-Object near-DL, near-IR spectrometer
Description

• Behind MOAO system
• Wavelength range 0.8-2.5µm
• Field of view 5 arcmin with multiple IFUs
• Image quality rms blur 0.015 arcsec
• Spatial sampling 0.05 arcsec over 2 arcsec
• IFUs 10
• Spectral resolution R2000-10000

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Multi-Object Intermediate-Resolution, Near IR
spectrometer Science

• Spectroscopy of distant galaxy matched to
  anticipated range of surface brightness aimed at
  deriving
• Stellar population mixes
• Kinematics
• for galaxies spanning a range of redshifts and
  environments
• Spectroscopy of the faintest objects (e.g.,
  first-light sources) in the near-IR
• JWST follow-up instrument

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Mid-IR Echelle Spectrometer Description

• Uses Mid-IR AO system
• Wavelength range 8-18µm
• Field of view 10 arcsec
• Slit length TBD
• Spectral resolution 5,000-100,000
• Notes at diffraction-limit, the background at
  these wavelengths is drastically reduced. JWST
  will not have a high-R mode.

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Mid-IR Echelle Spectrometer Science

• Physical structure and kinematics of protostellar
  envelopes
• Quantify mass accretion rate and envelope
  structure for forming stars spanning a range of
  masses
• Gas content and kinematics of circumstellar disks
• Constrain timescales for gas disk survival (giant
  planet building)
• Locate gaps and quantify masses and orbital radii
  of forming planets
• Kinematics and chemistry of obscured HII regions
• Kinematics and chemistry of envelopes ejected by
  evolved stars

18
Near-IR diffraction-limited Echelle Spectrometer
Description

• Uses small-field AO system
• Wavelength range 1-5µm
• Field of view 20 arcsec
• Slit length TBD
• Spectral resolution 20,000-100,000
• Think of NIRSPEC with a 30m collecting aperture
  and reduced sky via working at the diffraction
  limit with small slits (or equivalent IFU
  sampling).

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Near-IR diffraction-limited Echelle Spectrometer
Science

• Radial velocity studies of M-type stars aimed at
  detecting low-mass planets
• Studies of element and isotopic abundances
• Studies of stellar magnetic fields
• Kinematics of newly-formed stars in molecular
  clouds
• Kinematics of obscured stellar jets
• Physics of the IGM at z gt 5.5

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Extreme AO planet imager Description

• Contrast ratio
• first generation 106 _at_1.65µ for H 11 stars
• second generation 108 _at_1.65µ for H 8 stars
• Wavelength range 1-2.5µm
• Field of view 0.03?? to 1?? (4l/D- 20l/D)
• R 100 spectroscopic capability

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Extreme AO planet imager Science

• Initial targets self-luminous, young
  Jupiter-analogues
• Second generation targets Reflected-light
  planets, planet-forming environments
• Image planets (at spectral resolution 5 to 100)
  with the goal of characterizing albedo, radii,
  composition and approximate physical structure
• Image other high contrast scenes (AGN CS disks)

22
High resolution optical echelle spectrometer
Description

• Wavelength range 0.31-1.3µm
• Field of view 10 arcsec
• Image quality seeing limited
• Spectral resolution R50,000 with 1 arcsec slit

23
High resolution optical echelle spectrometer
Science

• Stellar abundance studies in the MWG and beyond
• Stellar seismology
• ISM abundances and kinematics
• Doppler imaging of stellar surfaces
• QSO absorption line studies (gain in potential
  targets is very large, factor of 100)

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Moderate field, near IR diffraction-limited
imager Description

• Likely classical MCAO system
• Wavelength range 0.8-5µm
• Field of View 30 arcsec
• Image quality diffraction limit
• Spatial sampling Nyquist sampling
• Spectral resolution 5-100
• Photometry 2
• Astrometry TBD

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Moderate field, near IR diffraction-limited
imager Science

• Deconstruction of stellar populations in galaxies
  out to 10 Mpc
• IMFs in dense star-forming regions
• Requires complementary DL-IFU spectra
• Astrometry of stellar orbits in the Galactic
  Center
• Astrometry of obscured clusters

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Instrument Summary
27

• Take home thoughts in the context of Keck
  Observatory
• First operational light (WFOS, mid-IR echelle)
  2015 at earliest
• Widest-field instrument will likely have FoV 10
  arcmin (diameter)
• No wide-field or seeing-limited near-IR
  capability planned
• In the diffraction-limited world, 30m is hard to
  touch for point-sources
• Pay attention to TMT UV capability. Current goal
  of 0.31µ may prove difficult to achieve
• Where will TMT be?

Wide-field seeing limited
AO at ? lt 800nm
Interferometry