Transcript TMT Science Overview - GSMT Program Office

Science with TMT
The Power of the Planned Instrument Components
GSMT SWG
August 10, 2006
Paul Hickson
The authors gratefully acknowledge the support of the TMT partner institutions. They are the
Association of Canadian Universities for Research in Astronomy (ACURA), the Association of
Universities for Research in Astronomy (AURA), the California Institute of Technology and the
University of California. This work was supported, as well, by the Canada Foundation for
Innovation, the Gordon and Betty Moore Foundation, the National Optical Astronomy
Observatory, which is operated by AURA under cooperative agreement with the National Science
Foundation, the Ontario Ministry of Research and Innovation, and the National Research Council
of Canada.
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The TMT
UC, Caltech, AURA, ACURA
Draws from three ELT design studies
– GSMT
– CELT
– VLOT
Unique aspects:
– 30-m filled circular aperture
– Wide 20 arcmin FOV
– A broad complement of
instruments
– Powerful adaptive-optics
systems
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Science and Instrument development
Science programs drawn from a wide community in the USA and Canada
12-member Science Advisory Committee
– identified 8 instruments and 4 AO modes
– Science Requirements Document
– Detailed Science Case
Instrument Feasibility Studies
– Independent teams develop designs and science programs for the
SAC instruments
– Non-advocate reviews for each instrument and AO systems
TMT Conceptual Design Review - May 2006
– “This is a well-scoped project, technically challenging, yet within
reach. It will enable a new era in astronomy that is seductive and
highly motivating.”
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TMT Aperture Advantage
Seeing-limited observations and observations of resolved sources
Sensitivity  D2 (~ 14  8m)
Background-limited AO observations of unresolved sources
Sensitivity  S2 D4 (~ 200  8m)
High-contrast AO observations of unresolved sources
2
S
Sensitivity  
D4 (~ 200  8m)
1 S
High-contrast ExAO observations of unresolved sources
Contrast  D2 (~ 14  8m)
Sensitivity  D6 (~ 3000  8m)
Sensitivity 1/ time required to reach a given s/n ratio
  throughput, S  Strehl ratio. D  aperture diameter
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TMT Adaptive Optics Modes
NFIRAOS - Narrow-field infrared adaptive optics system
– LGS MCAO system - two DMs and asterism of seven laser stars
– Diffraction-limited over 30 arcsec FOV
– 2 arcmin FOV for AO-sharpened tip-tilt & focus stars
– S ~ 0.5 at 1 um (S ~ 0.3 at first light)
– Passed conceptual design review, May 2006
TMT NFIRAOS Team
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TMT Adaptive Optics Modes
ExAO - Extreme adaptive
optics
– High-order AO system
– Diffraction suppression
system - two-stage
nulling interferometer
– Speckle suppression
system
108 contrast achieved on a simulated G5
star at 30 pc in 1 hr. (TMT PFI team)
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TMT Adaptive Optics Modes
MIRAO - Mid-infrared adaptive optics
– Conventional high-Strehl laser AO system
MOAO - Multi-object adaptive optics
– Deployable probes with MEMS deformable mirrors
– Open-loop correction determined from LGS asterism
GLAO - Ground-layer adaptive optics
– Image ‘sharpening’ (low-order correction) over a wide field of view
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IRIS
Near-infrared imaging
spectrometer
– ~ 15-arcsec FOV
diffraction-limited
imager (4 mas pixels)
– 0.8 - 2.5 um
– On-axis R ~ 4000
IFU spectrometer
– Employs NFIRAOS
MCAO system
TMT IRIS Team
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IRMOS
Infrared multi-object
spectrometer
– Multiple IFUs
accessing a 2 - 5
arcmin FOV
– 0.8 - 2.5 um
– R ~ 2000 - 10000
– Employs MOAO
to give neardiffraction-limited
resolution
CIT IRMOS Team
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WFOS
Wide-field optical
spectrometer
– 0.3 - 1.2 um
– R ~ 150 - 6000
– 8 - 20 arcmin FOV
– GLAO capable
TMT WFOS Team
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HROS
High-resolution optical
spectrometer
– 0.3 - 1 um
– R ~ 20,000 - 100,000
– Fiber feed MOS option
UC HROS Team
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MIRES
Mid-IR Echelle spectrometer
– 5 - 28 um
– R ~ 5000 - 100,000
spectrometer
– MIR slit-viewer / science
imager
– Employs MIRAO system
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NIRES
Near-infrared Echelle spectrometer
– bNIRES: 1 - 2.5 um
– rNIRES: 2.9 - 5 um
– diffraction-limited
– R ~ 20,000 - 100,000
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PFI
Planet formation instrument
– high-contrast (~ 108) ExAO
– 1 - 5 um 2” x 2” imager and IFU
spectrometer (R ~ 70 - 700)
TMT PFI Team
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Key advances enabled by TMT
Fundamental physics
– 10x improvement in search for variations of fundamental constants
First light
– Detect first-light objects and study their physical properties
Intergalactic medium
– Map ionization and chemistry from first-light to present
– Tomographic structure of IGM and gas-galaxy connection
Galaxy formation/evolution
– Determine morphology, kinematics, dynamics, chemistry of galaxies at all redshifts
with 5x the resolution of JWST
– Probe the dark matter distribution in elliptical galaxies
Black holes
– Study BH’s in all galaxy types and resolve the sphere of influence to z ~ 0.4
– Determine properties of the Galactic BH, the DM distribution, and test GR
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Key advances enabled by TMT
Stellar populations
– Determine the star formation history in galaxies as far as the Virgo cluster
Star and planet formation
– Measure the IMF over the full range of mass in a variety of environments
– Resolve bipolar outflows and study feedback to the IGM
– Measure accretion rates and relationship to mass of protostars
– High-resolution observations of planets and protoplanetary disks
Exoplanets
– 30x increase in Doppler detection of exoplanets
– Detect terrestrial planets in the habitable zones of M stars by Doppler shift
– Detect planets by reflected light
– Direct spectroscopy of massive planets
– Characterize exoplanet atmospheres by absorption spectroscopy
The Solar System
– Direct detection of sub-km TNOs
– Atmospheric and surface chemistry of outer solar system objects
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Cosmology and Fundamental Physics
- The nature of dark matter and dark energy
What is Dark Matter and Dark Energy?
Many theories - some predict variation
of fundamental parameters.
Wavelengths in multiplets of
redshifted UV lines in quasar spectra
are sensitive to   e2 / hc and to
  m p / me .
A decade of study with 10m-class
telescopes has hinted at variations:
– Mixed results for variation of .
– Tentative (3.5) evidence for
variability of .
HROS will provide a definitive
resolution.
Wavelength residuals seen in QSO
spectra vs. sensitivity coefficient.
Positive slope indicates variation of .
(Reinhold et al. 2006)
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The Early Universe and First Light
- The first luminous objects
TMT should detect the first
luminous objects - and will study
the physics of objects found with
JWST:
– Detection of He II emission
would confirm the primordial
nature of these objects.
– With IRIS and IRMOS, we will
be able to study the flux
distribution of sources, and
the size and topology of the
ionization region.
– IRMOS will reach ~ 2x10-20
erg s-1 cm-2 for 25 mas
sources in 4 hrs (an order of
magnitude fainter than JWST)
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Schaerer 2002
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The Intergalactic Medium
- Probing beyond z ~ 7
NIRES will use adaptive optics and infrared spectroscopy to probe the
evolution of the IGM beyond z ~ 7:
– CIV, OI, CII lines are not affected by the Lyman- forest.
– Gamma ray bursts could provide high redshift beacons.
Lyman limit
Lyb
Ly
SiII CII
SiIV
SiII CIV
Ly
Lybem
NV
CIV
SiIV
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The Intergalactic Medium
- Tomography of the baryonic structure
WFOS will use multi-object spectroscopy
of background galaxies to map the
structure of IGM during the peak epoch
of galaxy formation (z ~ 2 - 3.5).
– This will elucidate the relationship
between galaxies and the IGM.
Simulated TMT observation with R = 24
source galaxy (WFOS-HIA team).
Simulation of dark matter structure at
z = 3. (R. Cen, Princeton Univ.)
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Galaxy Formation and Evolution
- Detecting the first galaxies
IRMOS will be able to detect
galaxies at very high redshift:
– Ly- detectable to z > 12.
– z ~ 15 should be detectable
by placing IFUs on caustics
of gravitational lens
systems.
– Adaptive optics is critical
for these small objects.
There are potentially many
objects per TMT field of view,
depending on the transparency
of the intergalactic medium.
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TMT IRMOS-UFHIA team
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Galaxy Formation and Evolution
- Detailed mapping of high-redshift galaxies
IRIS and IRMOS will probe chemistry and dynamics of high-redshift
galaxies and study the assembly of galaxies with 100 pc resolution.
Multiple deployable IFUs will provide statistically significant samples.
Key questions:
– How does the age of the stellar population compare to the dynamical
age of the galaxy?
– How do star formation modes relate to the dynamical state?
– How do massive galaxies of old stellar populations form and evolve?
– How does the Hubble sequence arise?
– How do bars, bulges,disks form?
– How important is feedback?
J. Larkin
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Galaxy Formation and Evolution
- Physics of galaxy formation
IRIS and IRMOS will
map the physical state
of galaxies over the
redshift range where
the bulk of galaxy
assembly occurs:
z=0
– Star formation rate
– Metallicity maps
z = 2.5
– Extinction maps
– Dynamical Masses
– Gas kinematics
Synergy with ALMA:
z = 5.5
– Molecular emission
TMT IRMOS-UFHIA team
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Galaxy Formation and Evolution
- Dark matter distribution
WFOS can measure radial velocities for virtually all globular clusters in
Virgo cluster elliptical galaxies.
This will allow us to probe the dark matter distribution in these massive
galaxies.
M49
M49
TMT
Keck
TMT WFOS-HIA team
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Black holes and Active Galactic Nuclei
- Evolution and the galaxy - BH connection
IRIS will determine black hole
masses over a wide range of
galaxy types, masses and
redshifts:
– It can resolve the region
of influence of a 109 M
BH to z ~ 0.4 using
adaptive optics.
Key questions:
– When did the first supermassive BHs form?
– How do BH properties
and growth rate depend
on the environment?
– How do BHs evolve
dynamically?
– How do BHs feed?
CFA Redshift Survey galaxies
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Black Holes and Active Galactic Nuclei
- The galactic center
IRIS will map stellar orbits in
the galactic center with
exquisite precision:
– This will allow us to probe
the gravitational potential
and study the nature of
dark matter on small
scales.
– It will provide a precise
measurement of the black
hole mass, galactic
constants, and will detect
relativistic effects.
A. Ghez, UCLA
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Stellar Populations in the Local Universe
- Stellar archaeology
IRIS and HROS will determine
the star formation history in
galaxies out to the Virgo cluster:
– Adaptive optics will allow
photometry of resolved
stellar populations in
crowded fields.
Simulated M32 CMD with
TMT MCAO. The red, blue
and green lines represent
three input stellar
populations. (K. Olsen,
NOAO)
– This will give star-formation
history and metallicity in a
wide range of environments.
– High-resolution spectroscopy
will provide element
abundances.
– Complimentary to high-z
galaxy studies.
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Stellar Populations in the Local Universe
- Dynamics of halo stars
HROS will use multi-object
spectroscopy of thousands
of stars to map the
dynamical states of stellar
populations:
– This will allow us to test
theories of structure
formation on subgalactic scales.
– By comparison with
models, one can infer
the merger history of
nearby galaxies.
N-body simulations of satellite
accretion (TMT WFOS-HIA team,
Bullock & Johnstone 2005). TMT.PSC.PRE.06.032.REL01
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Evolution of Star Clusters and the IMF
IRIS will allow us to determine
the initial mass function in star
clusters from < 1 to 100 M in a
range of stellar environments:
– IFU imaging/spectroscopy at
the diffraction limit with
MCAO.
AO image of star field in M31 from
Gemini/Altair. TMT’s MCAO will provide
better psf uniformity, higher Strehl
ratios, 4x sharper images and ~ 20x
deeper imaging (TMT IRIS team).
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Physics of Star and Planet Formation
- Bipolar outflows
IRMOS will allow us to study the
physical conditions in starforming regions:
– Resolve bipolar outflows
using adaptive optics and
study their interaction with
the ISM in galactic starforming regions.
– Investigate feedback from
protostars to the molecular
cloud.
– Study many Herbig Haro
objects at a time using
deployable IFUs.
– Will compliment submm
observations with ALMA.
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Perseus star-forming region
(TMT IRMOS-CIT team)
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Physics of Star and Planet Formation
- Young stellar objects
NIRES will be able to
characterize essentially all
young stellar objects in
nearby star-forming
complexes:
– High-resolution spectra
of the CO fundamental
line will allow mass
accretion rates to be
derived.
TMT NIRES team
TMT flux limit (500s, R=100,000, s/n = 50)
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Physics of Star and Planet Formation
- Protoplanetary disks
MIRES will resolve the inner regions of protoplanetary disks to study
abundances, chemistry, kinematics and planet formation dynamics:
– Determine physical properties of the disk and detect gaps
produced by planets
– Synergy with ALMA, JWST.
G. Bryden & J. Najita
G. Bryden
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Physics of Star and Planet Formation
- Planet formation
MIRES will be able to
image protoplanetary disks
and detect features
produced by planets:
– TMT will have 5x the
resolution of JWST.
Simulation of Solar System
protoplanetary disk (Liou & Zook 1999)
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Doppler Detection of Extrasolar Planets
HROS will expand the
number of host stars
accessible to Doppler
spectroscopy by a
factor of ~ 30, and
provide sensitivity to
lower-mass stars
R. P. Butler
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Characterization of Extrasolar Planets
- Doppler detection
HROS will be able to
detect Earth-mass
planets in habitable
zones around
nearby M stars:
– M stars are the
most common
stars in the
galaxy. Their
habitable zone is
0.01 - 0.3 AU.
Kasting et al 1993
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Characterization of Extrasolar Planets
- Direct detection
PFI will directly image young planets near low-mass stars using
high-order adaptive optics (ExAO)
– Arguably the most technically challenging (and rewarding) of all
the TMT technologies
4 MJ planet orbiting a
brown dwarf
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~80 MJ planet orbiting
an old K star
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Characterizing Extrasolar Planets
- Extreme adaptive optics
TMTs large aperture
will allow detection of
planets closer to their
host stars:
– Detection of
planets by
reflected light.
– Probe scales
comparable to
inner Solar
System.
– Detect planets
forming in
circumstellar disks.
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TMT PFI team
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Characterizing Extrasolar Planets
- Properties of exoplanets
TMT will provide:
– Doppler follow-up of
transit detections
(HROS).
– Absorption
spectroscopy of
atmospheres of
transiting planets
(HROS).
– Reflected light
spectroscopy of “hot
jupiters” (PFI).
– Direct spectroscopy of
massive planets (PFI).
GJ 876d: 7.5 M
Lynette Cook
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Characterization of Extrasolar Planets
- Atmospheres of massive planets
MIRES will be able to
measure the spectra of
massive planets in the
mid-infrared:
– Contrast is lower in the
mid-infrared.
– Strong molecular lines
characterize the
atmospheric
composition.
– Spectral deconvolution
can reveal the planetary
spectrum
TMT MIRES team
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Characterization of Extrasolar Planets
- Atmospheres of terrestrial planets
TMT will detect the
absorption signatures of
gases in the atmosphere in
transiting planets.
– Na, K, He, will be easily
detectable with TMT
To Earth
O2 A-band
HROS should be able to
detect O2 in the atmosphere
of an Earth-like planet
orbiting in the habitable
zone of an M star
– s/n ~ 30,000 per 6 km/s
resolution element achievable by TMT in ~
3 hrs.
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Webb & Wormleaton 2001
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Solar System Studies
TMT will extend studies of the outer
Solar System:
– IRIS will be able to detect a 1 km
TNO at 50 AU in 15 min.
IRIS and MIRES will provide a capability
for high-spatial resolution imaging and
spectroscopy of planets and satellites of
the solar system:
– high-resolution spectra of features on
outer Solar System bodies will allow
studies of atmospheric physics and
atmospheric and surface chemistry
– Regular monitoring will allow TMT to
study transient phenomena, weather,
volcanic activity, etc.
Europa at the resolution of TMT
adaptive optics (M. Brown, CIT)
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Solar System Studies
-Atmospheric chemistry
MIRES will be able to
study the atmospheric
physics of the outer
planets and their
satellites by mapping
them at high spectral
and spatial resolution
using adaptive optics
– This resolution is
well beyond what
has been
achieved by
planetary space
missions.
High-resolution spectra of Titan. (Roe et al. 2003)
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Summary
TMT will open new frontiers over
a broad range of science areas.
This will be enabled by an
ambitious complement of
instruments and sophisticated
adaptive optics systems.
D4 gain will provide a 100-fold
increase in sensitivity compared
to 8 - 10 m telescopes, opening
vast new discovery space.
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