Luc Simard AO4ELT3 Conference Firenze, May 27-31, 2013

TMT.PSC.PRE.13.017.REL03

Luc Simard

AO4ELT3 Conference

Firenze, May 27-31, 2013

Exploring the Full Cosmic Timeline with TMT


TMT Cosmic Timeline - 13.3 Billion Years


Working at the Diffraction Limit

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Seeing-limited observations and observations of resolved sources

Background-limited AO observations of unresolved sources

High-contrast AO observations of unresolved sources

The Importance of Adaptive Optics

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TMT as an Agile Telescope:Catching The “Unknown Unknowns”

TMT target acquisition time requirement is 5 minutes (i.e., 0.0034 day)

Source: Figure 8.6, LSST Science Book

Tightly sequenced observations will be key

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From Science to Subsystems

Transients - GRBs/ supernovae/tidal flares/?Fast system response time

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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TMT.PSC.PRE.13.017.REL03 7

Summary of TMT Science Objectives and Capabilities


TMT Planned Instrument Suite


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

High-Contrast Exoplanet Imager TIGER PFI EPICS

Near-IR, AO-assisted Echelle Spectrometer

GMTNIRS NIRES SIMPLE

High-Resolution Optical Spectrometer

G-CLEF HROS CODEX

“Wide”-Field AO Imager WIRC MICADO


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

MCAO

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Vegetti et al. 2010


Towards Resolving the Missing Satellites Problem

Strigari et al. 2007

The TMT mass limit of 107 M is where the discrepancy is the largest!

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Inter-Galactic Medium Tomography: Now

(Simulation:M. Norman, UCSD)

SL

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SL

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Inter-Galactic Medium Tomography: TMT



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

SL

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Inter-Galactic Medium Tomography: TMT


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.

Schaerer 2002

MOAO

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Synergies I. First Light and Re-ionization

Penetrating the Early Universe with ionized bubbles

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

Source: IRMOS Caltech Feasibility Study

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High-Redshift Star Formation MOAO

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Synergies II. SKA

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

Spectroscopic limits (Padovani 2011)

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Physics of Galaxy Formation

TMT will use adaptive optics to map the physical state of galaxies over the redshift range where the bulk of galaxy assembly occurs:

Star formation rate

Metallicity maps

Extinction maps

Dynamical Masses

Gas kinematics

Synergy with ALMA:

Molecular emission

z = 0

z = 2.5

z = 5.5

TMT IRMOS-UFHIA team

MOAO

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Physics of Galaxy Formation

TMT will use adaptive optics to map the physical state of galaxies over the redshift range where the bulk of galaxy assembly occurs:

Star formation rate

Metallicity maps

Extinction maps

Dynamical Masses

Gas kinematics

Synergy with ALMA:

Molecular emission

z = 0

z = 2.5

z = 5.5

TMT IRMOS-UFHIA team

MOAO

TMT observations at z ~ 4 will be as good as current observations at z ~ 1

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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 contaminationTMT/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 contaminationTMT/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 MIRAO

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Resolved Stellar Populationsin 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 super-massive BHs form and feed?How do BH properties and growth rate depend on the environment?How do BHs evolve dynamically?

CFA Redshift Survey galaxies

TMT will expand by a factor of 1000 the number of galaxies where direct black hole mass measurements can

be performed

MCAO


Galactic Center

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.

MCAO

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Galactic Center with the IRIS Imager

17ʹʹ

100,000 stars down to K = 24

Courtesy: L. Meyer (UCLA)

K-band

t = 20sMCAO

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Substructures in Protoplanetary Disks

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)

MIRAO

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Synergies III. Planet Formation

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.

Figure 31“Science with ALMA” Document

TMT PFI:

106 @ 30 mas IWA(Taurus Jovians)

108 @ 50 mas IWA(Reflected light Jovians)

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Planet Formation and The Building Blocks of Life

Diffraction-limited, high spectral resolution observations in the mid-IR with TMT will probe complex molecules in

protoplanetary disks where terrestrial planets are expected to reside

MIRAO


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

VestaBinzel et al. 1997

Keck AO Zellner et al. 2005

MCAO


VestaBinzel et al. 1997

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

Geological Mapping of Asteroids


Observing Io with AO on TMT

Simulations of Io Jupiter-facing hemisphere in H band (Courtesy of Franck Marchis)

Keck/AO+NIRC2 Keck/NGAO TMT/AO+IRIS

TMT resolution at 1µm is 7 mas = 25 km at 5 AU (Jupiter)(0.035 AU at 5 pc, nearby stars)

MCAO


Simulations of Io Jupiter-facing hemisphere in H band (Courtesy of Franck Marchis)

Keck/AO+NIRC2 Keck/NGAO TMT/AO+IRIS

And:Methane rain fall on TitanThe geysers of Enceladus

Nitrogen geysers blowing in the wind on Triton

…

TMT resolution at 1µm is 7 mas = 25 km at 5 AU (Jupiter)(0.035 AU at 5 pc, nearby stars)

MCAOObserving Io with AO on TMT


Surface Mapping of Kuiper Belt Objects

F. Marchis (UC Berkeley/SETI)

Outstanding Questions:• Cryovolcanism• Bulk density and interior structure of the most primitive planetesimals

MCAO


Synergies VI. Solar System

Physics and Chemistry of Cometary Atmospheres

CO(2-1) emission and dust continuum from Comet Hale-Bopp at 1’’ resolutionwith with IRAM

Submm+optical = nucleus albedo and size

(Figure 40 - “Science with ALMA” Document)

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

Look for “chemical families” as probes of the Oort Cloud

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Strong Overlap Between Science and Instrumentation


Synergies VII. Space/IR and ALMA

The angular resolution of TMT instruments nicely complements that of JWST and ALMA

TMT/MIRES will have comparablespectral line sensitivity (NELF) to infrared space missions with a much higher spectral resolution

(TMT capabilities are shown in red)

TMT is a “near IR ALMA”!


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 world-class, next-generation facility

Strong synergies with ALMA, JWST, SKA, TESS and the time-domain (LSST, PAN-STARRS, …)

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Summary

Newly-established “International Science Development Teams” will now continue the work on TMT science


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.

Acknowledgments

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Luc Simard AO4ELT3 Conference Firenze, May 27-31, 2013

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