Transcript Slides - AO4ELT3

Exploring the Full Cosmic
Timeline with TMT
Luc Simard
AO4ELT3 Conference
Firenze, May 27-31, 2013
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TMT Cosmic Timeline 13.3 Billion Years
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Working at the Diffraction Limit
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The Importance of
Adaptive Optics
Seeing-limited observations and observations of resolved
sources
Sensitivity µ hD2 (~ 14 ´ 8m)
Background-limited AO observations of unresolved sources
Sensitivity µ hS2 D4 (~ 200 ´ 8m)
High-contrast AO observations of unresolved sources
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Sensitivity µ h S D4 (~ 200 ´ 8m)
1- S
Sensitivity =1/ time required to reach a given
s/n ratio
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= throughput, S = Strehl ratio. D = aperture diameter
TMT as an Agile Telescope:
Catching The “Unknown Unknowns”
TMT target
acquisition time
requirement is 5
minutes
(i.e., 0.0034 day)
Tightly
sequenced
observations will
be key
Source: Figure 8.6, LSST Science Book
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From Science to Subsystems
Transients - GRBs/
supernovae/tidal flares/?
Fast system response
time
NFIRAOS
fast switching
science fold
mirror
Articulated
M3 for fast
instrument
switching
Fast slewing
and acquisition
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Summary of TMT Science
Objectives and Capabilities
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TMT Planned Instrument Suite
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An ELT Instrumentation
“Equivalence Table”
Type of Instrument
GMT
TMT
E-ELT
Near-IR, AO-assisted Imager + IFU
GMTIFS
IRIS
HARMONI
Wide-Field, Optical Multi-Object
Spectrometer
GMACS
MOBIE
OPTIMOS
Near-IR Multislit Spectrometer
NIRMOS
IRMS
Deployable, Multi-IFU Imaging
Spectrometer
IRMOS
EAGLE
Mid-IR, AO-assisted Echelle
Spectrometer
MIRES
METIS
TIGER
PFI
EPICS
GMTNIRS
NIRES
SIMPLE
G-CLEF
HROS
CODEX
WIRC
MICADO
High-Contrast Exoplanet Imager
Near-IR, AO-assisted Echelle
Spectrometer
High-Resolution Optical
Spectrometer
“Wide”-Field AO Imager
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The Milky Way Halo According to
Cold Dark Matter
Dark matter particles
and NOT stars!
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Low-Mass CDM with Astrometric
Anomalies in Gravitational Lenses
TMT will be able to detect
astrometric anomalies in
gravitational lenses from
dark CDM haloes with
masses as small as 107
solar masses – a factor of
ten improvement
This will yield better
constraints on the nature of
the dark matter particle
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MCAO
Vegetti et al. 2010
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Towards Resolving the Missing
Satellites Problem
The TMT mass
limit of 107 M
is where the
discrepancy is
the largest!
Strigari et al. 2007
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Inter-Galactic Medium Tomography:
Now
SL
(Simulation:
M. Norman,
UCSD)
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Inter-Galactic Medium Tomography:
TMT
SL
(Simulation:
M. Norman,
UCSD)
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Inter-Galactic Medium Tomography:
TMT
SL
It will be possible to probe
individual galaxy haloes with
multiple sightlines
TMT is a wide-field telescope when
applied to the high redshift Universe:
20’ field of view is equivalent to 3.4
degrees at the redshift of SDSS
(Simulation:
M. Norman,
UCSD)
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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 TMT, we will be
able to study the flux
distribution of sources,
and the size and
topology of the
ionization region.
This will help us
understand how
reionization developed.
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MOAO
Schaerer 2002
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Synergies I. First Light and
Re-ionization
Penetrating the Early Universe with ionized bubbles
Source: IRMOS Caltech Feasibility Study
JWST: Detection of sources
TMT: (1) Source spectroscopy with IRIS/IRMS and (2) Mapping topology of bubbles around
JWST detections with IRIS/IRMS or IRMOS deployable IFUs
ALMA: Imaging of dust continuum up to z = 10 for complete baryon inventory
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High-Redshift Star Formation
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MOAO
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Synergies II. SKA
Spectroscopic limits (Padovani 2011)
The “Square Kilometer Array” will
probe the so-called Dark Ages
It will also survey sources at the
microjansky and nanojansky
levels
Expected to be optically very
faint
It will be possible with ELTs+SKA
to study star formation rates and
feedback from active galactic
nuclei in normal galaxies out to z
=6
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Physics of Galaxy Formation
MOAO
TMT will use adaptive
optics to map the physical
z=0
state of galaxies over the
redshift range where the
bulk of galaxy assembly
occurs:
Star formation rate
Metallicity maps
z = 2.5
Extinction maps
Dynamical Masses
Gas kinematics
Synergy with ALMA:
Molecular emission
z = 5.5
TMT IRMOS-UFHIA team
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Physics of Galaxy Formation
MOAO
TMT will use adaptive
optics to map the physical
z=0
state of galaxies over the
redshift range where the
bulk of galaxy assembly
occurs:
Star formation rate
Metallicity
z = 2.5 at z ~ 4 will be as
TMTmaps
observations
Extinction
goodmaps
as current observations at z ~ 1
Dynamical Masses
Gas kinematics
Synergy with ALMA:
Molecular emission
z = 5.5
TMT IRMOS-UFHIA team
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Merging galaxies often hidden behind gas and dust forming
stars – need mid-IR to penetrate extinction
High spatial resolution separates black hole region from host
galaxy contamination
TMT/MIRES will put JWST observations in context as done with
Spitzer and today’s 8m telescopes
–
At z=0.5, JWST resolution = 1.5 kpc and TMT = 330 pc
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Merging galaxies often hidden behind gas and dust forming
stars – need mid-IR to penetrate extinction
High spatial resolution separates black hole region from host
galaxy contamination
TMT/MIRES will put JWST observations in context as done with
Spitzer and today’s 8m telescopes
–
At z=0.5, JWST resolution = 1.5 kpc and TMT = 330 pc
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MIRA
O
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Resolved Stellar Populations
in Virgo Cluster galaxies
Requires:
• High Strehl
• PSF Uniformity
• PSF Stability
• Relatively large FoV
MCAO !
A 5ʹʹ x 10ʹʹ field in a Virgo Cluster galaxy spheroid observed with
an 8m telescope (left) and TMT (right) at the same Strehl ratio
(S=0.6) and an exposure time of 3 hours. Only the brightest
Asymptotic Giant Branch (AGB) stars are visible with an 8-m
telescope whereas TMT will probe down the Red Giant Branch
(RGB)
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Black holes and
Active Galactic Nuclei
TMT 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 and feed?
How do BH properties and
growth rate depend on the
environment?
How do BHs evolve
dynamically?
MCAO
CFA Redshift Survey galaxies
TMT will expand by a factor of 1000 the number of galaxies
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where direct black
hole mass measurements can be
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Galactic Center
MCAO
Mapping the orbits of stars at the Galactic Center with current Keck and
first-light TMT AO systems. Area shown is 0ʹʹ.8 x 0ʹʹ.8 (0.027 x 0.027 pc)
centered on Milky Way supermassive black hole. Wavelength is 2.1 µm.
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Galactic Center with the
IRIS Imager
K-band
t = 20s
MCAO
100,000 stars
down to
K = 24
Courtesy: L. Meyer
(UCLA)
17ʹʹ
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Substructures in
Protoplanetary Disks
MIRA
O
TMT will be able to image
protoplanetary disks and
detect features produced by
planets with mid-infrared
adaptive optics:
TMT will have 5x the
resolution of JWST.
Simulation of Solar System protoplanetary
disk (Liou & Zook 1999)
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Synergies III. Planet Formation
TMT PFI:
106 @ 30 mas IWA
(Taurus Jovians)
108 @ 50 mas IWA
(Reflected light
Jovians)
Figure 31
“Science with ALMA”
Document
Simulation of a protoplanetary system with a tidal gap created by a Jupiter-like planet at
7 AU from its central star as observed by ALMA
TMT’s Planet Formation Instrument (PFI) will allow detection of the planets themselves
that are responsible for the gaps and thus enable measurements of mass, accretion rate
and orbital motion.
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Planet Formation and
The Building Blocks of Life
MIRA
O
Diffraction-limited, high spectral resolution observations in
the mid-IR with TMT will probe complex molecules in
protoplanetary disks where terrestrial planets are expected
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to reside
Synergies IV. Proto-Star Formation
High-velocity outflowing gas in CO towards
protostar SVS13 (Keck/NIRSPEC)
TMT/MIRES will measure warm, dense
molecular gas to probe the base of
outflows in a large number of low-mass
protostars
Low-resolution Spitzer spectrum shows
exceptionally strong molecular absorption.
HCN and CO suggests gas originates in
an outflow
TMT/MIRES will measure molecular
abundances to determine the launch point
of the wind
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Direct Imaging of
Mature Exoplanets
ExAO
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Direct Imaging of
Mature Exoplanets
ExAO
Observing mature planets in
reflected light will tell us how many
planetary systems actually share the
same “architecture” as our own
Solar System.
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Synergies V. TESS
“Transiting Exoplanet Survey
Satellite”
Survey area 400 times larger
than Kepler’s
2.5 million of the closest and
brightest stars (G, K types)
2,700 new planets including
several hundred Earth-sized
ones
Planned launch: 2017
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Geological Mapping of
Asteroids
Keck AO
Zellner et al.
2005
MCAO
Vesta
Binzel et al. 1997
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Geological Mapping of
Asteroids
Keck AO
Zellner et al.
2005
TMT can resolve the surface of over
800 Main Belt asteroids
A MB asteroid will typically take ~2
hours to tumble across the
NFIRAOS field of view
Vesta
Binzel et al. 1997
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Observing Io with AO on TMT
Keck/AO+NIRC2
Keck/NGAO
MCAO
TMT/AO+IRIS
Simulations of Io Jupiter-facing hemisphere in H band (Courtesy of Franck Marchis)
TMT resolution at 1µm is 7 mas = 25 km at 5 AU (Jupiter)
(0.035 AU at 5 pc, nearby stars)
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Observing Io with AO on TMT
MCAO
And:
Methane rain fall on Titan
The geysers of Enceladus
Nitrogen geysers blowing in the
wind on Triton
…
Keck/AO+NIRC2
Keck/NGAO
TMT/AO+IRIS
Simulations of Io Jupiter-facing hemisphere in H band (Courtesy of Franck Marchis)
TMT resolution at 1µm is 7 mas = 25 km at 5 AU (Jupiter)
(0.035 AU at 5 pc, nearby stars)
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Surface Mapping of
Kuiper Belt Objects
MCAO
Outstanding Questions:
• Cryovolcanism
• Bulk density and interior
structure of the most
primitive planetesimals
F. Marchis (UC Berkeley/SETI)
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Synergies VI. Solar System
Physics and Chemistry of Cometary Atmospheres
CO(2-1) emission and dust continuum
from Comet Hale-Bopp at 1’’ resolution
with with IRAM
Submm+optical = nucleus albedo and size
Detection of parent volatiles in Comet Lee (C/1999 H1) at R=20,
000. TMT/NIRES will allow diffraction-limited observations at
R=100,000 over the range 4.5 - 28 µm
(Figure 40 - “Science with ALMA”
Document)
Look for “chemical families” as probes of the Oort Cloud
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Strong Overlap Between Science
and Instrumentation
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Synergies VII. Space/IR
and ALMA
(TMT capabilities are shown in red)
TMT/MIRES will have comparable
spectral line sensitivity (NELF) to
infrared space missions with a much
higher spectral resolution
The angular resolution of TMT
instruments nicely complements that
of JWST and ALMA
TMT is a “near IR ALMA”!
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Summary
TMT science programs span the full cosmic timeline:
From the “Dark Sector” and First Light
Including our own Solar System!
TMT has a powerful suite of planned science instruments
and AO systems that will make the Observatory a worldclass, next-generation facility
Strong synergies with ALMA, JWST, SKA, TESS and the
time-domain (LSST, PAN-STARRS, …)
Newly-established “International Science Development
Teams” will now continue the work on TMT science
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Acknowledgments
The TMT Project gratefully acknowledges the support of the
TMT collaborating institutions. They are the Association of
Canadian Universities for Research in Astronomy (ACURA), the
California Institute of Technology, the University of California, the
National Astronomical Observatory of Japan, the National
Astronomical Observatories of China and their consortium
partners, and the Department of Science and Technology of
India and their supported institutes. This work was supported as
well by the Gordon and Betty Moore Foundation, the Canada
Foundation for Innovation, the Ontario Ministry of Research and
Innovation, the National Research Council of Canada, the
Natural Sciences and Engineering Research Council of Canada,
the British Columbia Knowledge Development Fund, the
Association of Universities for Research in Astronomy (AURA)
and the U.S. National Science Foundation.
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